text:
Senior Community Specialist (planner Iv), Office Of Environmental And Energy Coordination
Construction and Skilled Trades, HVAC
Government and Public Services, State & Local
Under general supervision of the Assistant Director for Policy and Accountability within the Office of Environmental and Energy Coordination (OEEC), this position leads the Community Planning and Programs team in the promotion of environmental and energy awareness and engagement in support of the Board of Supervisors' Environmental Vision and Operational Energy Strategy. Responsibilities include, but are not limited to:
Grows and markets existing and new education and outreach programs to all community sectors;
Works with non-profit entities to further County goals;
Responds to inquiries from interest groups and the public;
Manages the CECAP (Communitywide Energy and Climate Action Planning) effort;
Works with departments/agencies to optimize energy and resource conservation through recovery and reuse;
Provides administrative support to the Board of Supervisors' Environmental Committee and the Environmental Quality Advisory Council (EQAC);
Provides leadership and general supervision for two positions, the Environmental Specialist and the Community Specialist.
Illustrative Duties
Manages complex, multi-faceted planning studies with citizens, County staff, other jurisdictions, State and/or Federal government;
Manages special projects and studies, including directing the work of a team or work group of planners and planning technicians or others, from within and outside of the Department to include contracting consultants, preparing schedules, and administering the project budget;
Represents the Department or County and serves as an internal expert on panels, committees, and task forces and may propose planning policies and amendments to the Comprehensive Plan in response to a variety of complex policy and issues;
Represents the Department's positions at public hearings before the Board of Supervisors, Planning Commission, and/or Park Authority Board, among others;
As representative of the Department, coordinates with other County agencies, interest groups, and jurisdictions on highly specialized policy issues;
Prepares detailed position papers and staff reports on complex proposals, environmental policy, among others;
Reviews and provides comments and direction on the work of others in related area of expertise, acting as an internal consultant to the department and a mentor to other planners;
Responds to complex land use, planning, and requests for interpretations or determinations;
Supervises advanced and complex planning work;
Serves as expert witness in litigation involving particular area of expertise.
Required Knowledge Skills and Abilities
Thorough knowledge of local government areas of specialization, including planning, management procedures, and principles of supervision;
Ability to write, proofread, edit, and rewrite documents effectively and to critique and edit the work of others;
Ability to apply interpersonal skills to resolve conflicts and to maintain effective communication with staff;
Ability to establish and maintain good working relationships with co-workers, elected and appointed officials, development representatives and citizen groups;
Ability to apply principles of leadership, creative problem solving, collaboration, decision making, and team building;
Ability to communicate effectively, both orally and in writing.
Any combination of education, experience, and training equivalent to the following: Graduation from an accredited four-year college or university in a planning-related field; plus five years of experience in a specific area of assignment or concentration, including, but not limited to, multi-layered, cross-agency zoning application evaluation, environmental policy, historic preservation, housing policy, public facility policy, and/or land use policy and implementation. A Master's degree may be substituted for one year of the required experience.
Master's degree in a related field. Senior-level experience and knowledge of energy and climate action planning including but not limited to areas such as greenhouse gas impacts and the impact of building energy and transportation emissions on the environment. Experience in developing and implementing a strategic plan as it relates to environmental and energy related issues. Experience working in a local government environment including work with elected officials. Significant demonstrated experience in data gathering techniques including how to manage, synthesize and use information in various formats and how to organize and present findings. Ability to work with community organizations including understanding and recognizing how to interact with the community at large. Ability to set-up and facilitate meetings. Ability to present information to elected officials, senior management, and members of the community in a concise and understandable manner. Ability to write clearly, synthesize complex information, and present findings to audiences without technical backgrounds. Ability to manage consulting contracts including the development of the scope of work for services and tracking and reporting on the progress of the work.
NECESSARY SPECIAL REQUIREMENTS:
The appointee to the position must satisfactorily complete a criminal background check as a condition of hire or continued employment.
Sufficiently mobile to attend offsite meetings both during and after normal working hours and to make presentations.
This position is primarily sedentary in nature; however, visual acuity to work on electronic equipment such as a computer monitor and typing on a keyboard are essential to the position. Ability to lift up to 15 pounds. All duties performed with or without reasonable accommodations.
Panel interview; candidates may be asked to complete written exercises and provide work samples.
Effective July 6, 2019, compensation plans will be increased by 2.1% (market rate adjustment.) Information here .
It is the policy of Fairfax County Government to prohibit discrimination on the basis of race, sex, color, national origin, religion, age, veteran status, political affiliation, genetics, or disability in the recruitment, selection, and hiring of its workforce.
Reasonable accommodations are available to persons with disabilities during application and/or interview processes per the Americans with Disabilities Act. Contact 703-324-4900 for assistance. TTY 703-222-7314 . EEO/AA/TTY.
Construction and Skilled Trades State & Local jobs in Fairfax
HVAC State & Local jobs in Fairfax


I recently moved and now that my horses have been in their paddocks a while the dirt has turned to powder. I've installed feed bins so they are not eating it and I wet it down daily however it dries out quickly and is extremely dusty. What can I mix with this powder to eliminate this dusty situation? I'm thinking of putting gravel into their shelters. Thank you.
Dust in the summer becomes mud in the winter. Come winter all those bare dusty spots will likely turn into mud so you do want to tackle this problem now. Fortunately, there are some low-tech solutions for avoiding dust and soil erosion: cover bare spots with some type of footing. Where you can, growing something to hold onto the soil is the best solution. This might be dryland grass (species of grass that are tolerant to low levels of rainfall) in the non-irrigated areas. In areas where you get rainfall or irrigation it might be trees, shrubs or native plants. If it's pasture, then plant pasture grasses.
For sacrifice areas, like paddocks and turnouts, cover with some type of crushed rock or other footing material — gravel, sand or chipped wood — wherever possible.
For more specifics you might check my Horses for Clean Water website. I have lots of resource materials there as well as Tip Sheets for sale for a small fee on different topics, including footing choices.


Most hedges are the responsibility of the person who owns the land next to the road. If the council, during a routine inspection, receive a complaint that hedges are overhanging a road or pavement, they will ask the landowner to cut them back. If the landowner fails to do this they may serve a formal notice. The owner could face legal action from an injured member of the public.
Check trees regularly, diseased or dead trees can be a danger.
 Does your hedge restrict the width of the pavement?
 Are people forced to walk at the edge of the pavement, or even on the road?
 Do trees on your land overhang the road?
 Do trees have a preservation order on them?
Think about the effect this has on all highway users.
Overhanging branches are a hazard for buses, lorries and pedestrians; particularly the blind, elderly and people in wheelchairs and mobility scooters/buggies.


The Global Alliance for Literacy within the Framework of Lifelong Learning (GAL) seeks to bring together key stakeholders and partners committed to building a more literate world through synergistic, innovative action. It will be launched by the Director-General of UNESCO on 9 September 2016 at UNESCO Headquarters in Paris, during this year's International Literacy Day celebration.
This initiative will be coordinated by the UNESCO Institute for Lifelong Learning (UIL) in Hamburg, and comprises the UNESCO Member States, inter-regional organisations, United Nations' (UN) specialised agencies and institutes as well as donors, participants from the private sector, civil society and others. Participation in the Alliance will be based on the commitment to contribute to a coherent action plan designed to foster literacy and sustainable development. GAL will, as a multi-stakeholder partnership, stimulate and promote collaborative programmes which connect literacy with the 2030 Agenda for Sustainable Development Agenda.


text:
J. B. (Phill) Parmer
J. B. (Phill) Parmer, 101, of Canyon, TX died of natural causes on December 30, 2020.
Graveside services will be held at 11:00 A.M., Saturday, January 2, 2021, at Memorial Park Cemetery. Military Rites will be provided by Volleys for Veterans. Arrangements are by Boxwell Brothers Funeral Directors, 2800 Paramount Blvd.
J. B. (Phill) Parmer was born on April 6, 1919, in rural Bell County, Texas, the son of Cicero Guess Parmer, a cotton sharecropper, and Ida Mae Ray.
He was a World War II veteran, serving in both the Army and Navy, in the Philippines, the North Atlantic, and in Italy. He received the Bronze Star medal for heroic service in a combat zone. He married Lorna Shannon Black in 1945 in Amarillo after writing to her throughout the war. He worked for Colorado Interstate Gas Company at Bivins, Texas for 35 years. He was an elder in the Church of Christ. He retired in 1983 to Sunrise Beach on Lake LBJ. In retirement he did the following: earned his EMT certificate and helped start the EMS service at Sunrise Beach; earned a paralegal certificate and became a member of the Silver-Haired Legislature of Texas, an advocacy group for seniors; worked as a senior care ombudsman, serving in the greater Austin area; studied and built several computers. He received The Greatest Generation award for his military service and volunteerism. He was a long-time member of Highland Lakes Church of Christ in Kingsland.
He is survived by his wife, Lorna of Canyon, TX; his son, Phill and wife Mevanee of Amarillo, TX; three grandchildren, Penelope Westwater of the St. Louis area, Shannon Butler of Philadelphia, and Cory Parmer of Davis, CA; and five great-grandchildren.
He was preceded in death by his parents; his son, Norman Duane; and his eight older siblings, Maybell, Doyle, Ivan, Ray, Vivian, Wilson, Ruthann, and Lawrence (Jick).
Memorials may be made to the Christian Relief Fund of Amarillo, Texas.
2 Replies to "J. B. (Phill) Parmer"
Marcello Biava says:
Sgt J.B. Parmer was in Company A, 473rd Infantry Regiment in Italy, during WWII.
His unit went through some of the thougest fighting of the war breaching the German held Gothic Line in Tuscany and Liguria.
On april 13th, 1945, his Battalion, started the bloody uphill attack against Hill 366 with "B" Company on the left, "A" Company on the right and "C" Company in reserve. It was planned to commit "C" Company in the attack later that day, and the morning was spent patrolling and planning. "A" and "B" met considerable opposition and were slowed to a crawl. "C" Company was committed at noon… Opposition half way up the first hill consisted of rifle, machine gun and rifle grenade fire. Potato-masher grenades and a mortar barrage were thrown in by the enemy for good measure. All of this was despite the artillery preparation made for the 1st Battalion's attack. Sniping from trenches and dugouts seriously wounded several men and killed or wounded the aid men who went to help him. The machine gun positions were taken after a number of enemy were killed or taken prisoner.
Three houses on a road parallel to the base of the hill were taken after a 20-minute firefight. Then the men were held up by machine gun and rifle fire after they had advanced within 300 yards of the church at S. Lucia. There they were was stopped by barbed wire and machine gun fire. Bangalore torpedoes were not available and they had to fall back to the company's defense line on the road crossed earlier that afternoon.
A mortar barrage on this defensive setup killed almost every S-Sgt in "C" Company. Leaderless platoons were combined when, with all the officers killed or wounded, the company commander, 1st Lt. Clarence E. Doughty was the only officer left.
On the 14th the
attack continued but gained no important headway. Sgt. Foster C. Eaton assumed command of 2nd Platoon when T-Sgt. Pustka was wounded.
On the morning of the 14th five enemy machine guns were delaying the advance of both battalions near Fontia. With "A" in support what was left of "B" Company worked up hill 427 at about 11 AM and got within a short distance of the guns when Jerry opened up and pinned them down. 1st Lt. Thomas A. O'Boyle, Company Commander, succeeded in getting his troops out of their exposed positions and regrouped for a second assault.
After two hours of perilous movement he had managed to get within 20 yards of the machine guns to direct a mortar barrage. Then, as so frequently happens in combat, things didn't go according to the book — smoke rounds from the barrage fell in the midst of "F" Company on the flank. Casualties from the short rounds were heavy and threatened to completely disorganize the
attack. Lt. O'Boyle visited his squads, encouraged and directed the continuance of the attack and directed the care and evacuation of the wounded.
The attack on these positions had begun at 11 AM and it was a bitter, bloody' and discouraging day cleaning out the machine guns but at 5 PM the job was done. Fontia was clear of enemy. A few hours later this advance coupled with other advances by the 2nd Battalion and assisted by the 1st Battalion's pressure on S. Lucia forced the enemy in the 2nd Battalion's sector to withdraw through Ortonovo to Casano and the hill behind it.
Before dawn on the 15th "A" Company was committed again and launched an attack on Hill 366, passed to the left of the troublesome barbed wire, and had a terrific fire-fight for the church on the crest of the hill at S. Lucia. German survivors fell back to dugouts and trenches on a knoll 100 yards away. Lt. Col. Phelan, 1st Battalion Commander who had spent his three days as CO in the most forward positions, moved to the church and directed the battle from there.
About noon, one squad was given the mission of rushing the enemy position. They ran through the heavy fire and practically onto the Germans. They forced one captured German to tell his comrades to surrender by marching him along at gunpoint to each trench and dugout netting 52 prisoners in this skirmish while losing only two wounded. Before the position was completely consolidated the enemy threw in a heavy mortar and artillery barrage.
One of these rounds landed in the church doorway and killed Lt. Col. Phelan, several "A" and "C" Company men and some PW's. Despite the losses, S. Lucia, a key observation point in the Green Line II was taken.
The men who fought on Hill 366, are now dead or in their 100s, wrinkled and often moving with the help of a cane or wheelchair. Their hands often tremble and their voices shake as they labor to speak. But nearly 80 years ago they were young men, many in their teens, fighting in a war to free a land that wasn't theirs, several thousands miles from home.
They may have been scared but they were also determined to do their jobs and perhaps more importantly not let down the man, the buddy, the friend fighting beside them.
Commemorate their Sacrifice, let everyone know their feats…
The people living in the villages these men have liberated.
sarah hancock says:
our dear friend. we have a pic of him and freind sitting with my husband at church in kingsland. he was a dear for sure. blessing to all the family, hugs to lorna. we love the Parmer family. harold and sarah hancock, burnet texas
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redpajama_set_name: RedPajamaCommonCrawl


To have hot water, you need to fit a 30, 40 or 50 gallon water heater depending on the everyday water consumption. Constant issues with hot water supply can be very annoying so a professional hydraulic company's set right may be the solution to the mess If broken pipes have deprived you of the pleasures of hot water in your shower, contact a craftsman plumber If hot water is not working in your dwelling in Sutton SM5, the best thing to do is get in touch with us and have it fixed for you.
If there is no hot water in your residence in Sutton SM5, phone us, we will books out the problem for a interesting fee If you are living with water leaks from a tap or hot water problems in your kitchen or bathroom in Sutton SM5, look no further and phone us. If only cold water runs from your tab and hot water is nowhere to be located don't wait around and call one of our trusted skilled plumbing experts Sometimes the indications of a faucet for hot water and cold water are the wrong technology round, and you need to call in a qualified plumbing professional to mend it. The shower head optimizes the stream of hot water and as a result, could save you a considerable amounts of money every year.
Depending on how dozens of harassing chasing in a household hot water consumption changes so the bigger the household, the bigger the water heater should be.


This weekend we're beginning a series called "Homewreckers," in which we're going to look at some of things that corrode our relationships and destroy our homes. For the last several years, about once a year, I have done a series on relationships.
I realize many in our church are not married; some of you hope one day you will be married and some of you don't. So, our team works really hard to make sure this is beneficial for all of you. Bottom line is, I think if you're single you'll get as much out of it as our old married folk, because we're learning principles about relationships, one form of which is marriage.
We're going to start this series in somewhat of an unusual place. I'm going to talk for a couple of weeks of how we walk with God in our jobs. Here's why. For many of you, especially you men, your home life is out of whack because your work life is off kilter as well.
Think about it this way. What is the source of a lot of the stress you bring into your home? WORK. You are dissatisfied at work; money is tight; you're under a lot of pressure; and you take that out on your family. Also the majority of your adult life is spent at work. To be honest, I think the church has done a patently bad job at teaching people what it means to follow Jesus in the workplace. Sometimes we talk about working for God as if it's a half-hour of something we're supposed to do on the weekend when you volunteer to be an usher. Volunteering at the church is important, but that's kind of like doing the chores around the house. For many of you, you should treat your workplace as your primary avenue for ministry. I've often pointed out to you that 37 out of 40 miracles in Acts take place not inside the temple, but out in the market place. That's a lot of miracles in the workplace!
So, over the next few weeks I want to teach you a little bit of what it means to be a believer in your workplace. Here's specifically the subject for this weekend: the role of ambition in your life. Here is a link to the manuscript.
But there is another kind of ambition that is good and right. It was the kind that led David to expand the borders of Israel; for Solomon, to build the Temple; for Nehemiah, to rebuild the walls; and for Paul, to spread the gospel to the ends of the earth. Paul even said, "I make it my ambition…" (Romans 15:26). That's the good kind. And Jesus was driven by an unparalleled ambition. The Gospels say, "Zeal (or, you could translate that 'ambition,' for your house has eaten me up") (John 2:17). And we're ambitious as a church. Our goal is to plant 1000 churches in the next 40 years all over the world.
Yes, selfish ambition has caused greedy executives to exploit the poor and ruin our economy; selfish ambition has driven some dictators to send nations to war; selfish ambition has made some men and women destroy their families and neglect their children.
But in our reaction to that we don't need to get rid of all ambition. We need to redeem it. We need to rescue it. We live in a world desperately in need of people who are ambitious for the right things… godly things.
And don't think, by the way, that if you're not aggressive, a firstborn, or a natural leader, that you're not ambitious. We all have goals, and we're all ambitious to see them met in our own way. Some of you want to be married, and so you're ambitious for that. Some of you strongly desire to have a family. You want your kids to turn out well. You want a comfortable life.
Unless you have no wants, no needs, no desires, you have no ambitions. And if you have no wants, needs, or desires… you're dead.
I look forward to getting into the message this weekend called "Redeeming Ambition," from Philippians 4:11-13. I'll show you what godly ambition looks like, and give you some litmus tests you can take to see if your ambition is godly or selfish. I have learned a lot about this from a book I read last year by Dave Harvey called Rescuing Ambition. I hope you'll make it part of your summer reading list.


Contemporary Kitchen Window Treatments HGTV Pictures was posted in December 8, 2018 at 9:43 pm. Contemporary Kitchen Window Treatments HGTV Pictures has viewed by 28 users. Click it and download the Contemporary Kitchen Window Treatments HGTV Pictures.


text:
class BaseModel {

    /**
     * constructor
     *
     * @param {Boolean} sync syncronization switch
     */
    constructor(sync = false) {
        (async () => {
            await this.syncModel(sync);
        })();
        return this.schema;
    }

    /**
     * return schema
     */
    get schema() {
        return this.getSchema();
    }

    /**
     * return schema name
     */
    get schemaName() {
        return this.constructor.name;
    }

    /**
     * to sincronize model with table
     *
     * @param {Boolean} sync syncronization switch
     */
    syncModel(sync) {
        return new Promise(async (resolve, reject) => {
            try {
                if (sync) {
                    await this.schema.sync({ force: false });
                    console.log(`${this.constructor.name} sincronized!`)
                }
                resolve(true);
            } catch (error) {
                console.log(error);
                reject(error);
            }
        })
    }

}

export default BaseModel;

redpajama_set_name: RedPajamaGithub


Aforsima Leather Sectional Sofa is an L-shaped modular seating program that can be easily adapted to new classic-contemporary living. It is a dynamic Italian sofa where each element takes part to set up an original interplay of soft volumes. This incredibly comfortable and stylish design with chunky arms comes in tan leather upholstery done on solid wood frame and legs.
The large and cosy features of our much-loved Aforsima give modern look and feel. This luxurious and deep-seated sofa is a fantastic choice for any contemporary-styled home. Feather-filled backrest with separated sections.


text:
in: Stu, Other Fandoms
Tybalt is a minor character from Shakespeare's Romeo and Juliet, although he is based off the musical version, the Hungarian one in particular, because it owns. Originally made by Renn, he has been adopted by Sarrin. Most of his plot is from his time with the former.
1 Background and History
1.1 Paris
1.2 Appearance and Personality
2.1 Mercutio
2.2 Meg
2.3 What was the "Appearance and Personality" section before I made this profile serious
Background and History[]
The Montagues and the Capulets (although Tybalt would probably render it thusly: The Capulets and the Montagues) have beha gayyyyyyyyyyyyyyyyyyyyyyymber (although, funny enough, not one remembers why), and their hatred distorts the lives of their children more than it affects them. Sexy Tybalt is not actually a Capulet himself except by law; his father's younger sister became Lady Capulet by marriage and convinced her husband to adopt him. Tybalt's memory of his parents is dim, but he has never quite come to see his adopted parents as parents at all. He is not referred to as a son by them, which might have something to do with it.
From a young age - although not from birth; his parents themselves raised him away from the feud until they died, when he was seven - he was trained to defend Capulet's honor, which he does admirably, although as anything other than a duellist he fails miserably, and knows it. His intense love for his aunt - and his even more passionate love for his cousin - are both totally unrequited. (The latter has furthermore been suppressed in response to her marriage to Romeo Montague.) In Verona, he'd only ever been with a woman paid to do so.
He is an epileptic. This is due to an injury incurred during an early accident horse-riding; for a very long time Tybalt, who had been terrified of horses as a child even before this incident, hated the animals. (Tybalt hated a lot of things when he was young.) His horse is currently one of the only things he feels any tenderness for - at least, the kind he's willing to show.
It would be a simplification to say that he loathes himself.
Paris[]
Tybalt undoubtedly mumbled something incomprehensible about his reasons for going to Paris, but the simple truth of it is that his cousin Julia recently dishonored the family and broke his heart by marrying his mortal enemy*, and he would have liked nothing more than to forget he ever looked on her. Paris, however, holds many distractions, one of them in the shape of a buxom ballerina named Meg Giry, and the other irritatingly familiar as Mercutio. Although he's starting to figure out the shape of Mercutio, too, in a way he'd have never guessed with the man's clothes on.
((*I know this is not what was played, but it's the only reason I can think of for him to leave Paris.))
Appearance and Personality[]
Tybalt is tall and wiry, well-built and athletic, although when he is not directing his energy into his considerable skill with fighting, he does not seem to know how to move, and there is something odd and erratic about his motion. He is rather beautiful in a striking, intense way, with dark looks and a strong presence; he is generally oblivious to this, as might be expected.
He has repressed more or less most everything about himself and tends to be broody and despairing; his temper is short and he is quick to rage, because rage is one of the only feelings he can express and allow himself to unwind in. The only things he is comfortable with are those staples of his feud-themed upbringing, and yet, despairing of that, too, they do not give him much pleasure without simultaneously delivering its opposite. Paris has led to some - to his mind - unsavory side-effects. While he is outside of Verona's hate-charged atmosphere he is in some ways finding a new beginning, but this, unfortunately, also makes him think, and it is very hard on him for him to challenge his rigid notions of the world.
Plot[]
Mercutio[]
Mercutio is the bane of Tybalt's existence. He is also really, really, ridiculously amazing in bed. Tybalt is not pleased by this.
It's not love unless you actually express it through attempted bone-breaking, right?
Except, um, when he is.
Tybalt thinks more than Mercutio (and talks less), but he does not always like what he finds. When he finds himself coming to the conclusion that there could be tenderness intimacy something other than hate anything less than oh-so-rigid animosity between them, he represses the thought. (Yeah, that was a pun.)
Meg[]
Tybalt met the ballerina Meg Giry at a dance. If either was capable of knowing what love is, it might have been love at first sight. Their courtship has been awkward, but persistent, and with more cute moments than anyone knows what to do with.
Meg performing. Tybalt has probably seen more of her performances than she is aware of.
Tybalt does think he genuinely loves Meg, but he is convinced she could never love him; his own self-loathing means he thinks himself unworthy of her. Any physical expression of intimacy between them is always abruptly canceled out by this.
What was the "Appearance and Personality" section before I made this profile serious[]
It occurs to me that if the personality were different, Tybalt might dress more snazzily, more sexily, in perhaps more tank tops, more daring pants, with bracelets or a ponytail or somesuch gloriousness. He might also slink around in a more feline manner and exude even more intimidating badassery than he already does. Actually, he would be very similar to his nemesis and sometimes-loverbedfellow Mercutio.
But Tybalt's personality is not different. It is repressed.
REPRESSED REPRESSED REPRESSED
He's still a babe, though.
Other inside jokes and the like can be found at the comical Mercapulet page. Hey, considering how much misery is going to take place in this plot, they deserve a comical page.
3 Blind Mag


text:
\section{Introduction}

Be/X-ray binary pulsar GX~304-1 was discovered during hard X-ray sky surveys
with balloon observations in 1967 (McClintock et al. 1971). The X-ray source
was detected with successive space missions and recognized as 3U~1258-61,
4U~1258-61 \& 2S~1258-613 (Giacconi et al. 1974; Bradt et al. 1977;
Forman et al. 1978). Using data from $SAS-3$ observations, X-ray pulsations
at $\sim$272~s were discovered in the source (McClintock et al. 1977).
Spectral investigation of the pulsar, carried out from balloon observations,
showed that the continuum spectrum in 18-35~keV range was described by a
power-law (Maurer et al. 1982). Later, a power-law model modified with high
energy cutoff was used to explain the 2-40~keV continuum spectrum obtained
from  $HEAO~1$ observation of the pulsar (White, Swank \& Holt 1983). Analyzing
the periodicity of the X-ray outbursts in 7 years of data from $Vela~5B$, the
orbital period of the GX~304-1 was reported to be 132.5~d (Priedhorsky \&
Terrell 1983). A shell star with visual magnitude of 15 was discovered in
the X-ray error box of the neutron star and identified as the optical
companion of the pulsar (Mason et al. 1978). High resolution optical
spectroscopy established the spectral class of the companion as Be star
of type B2~Vne which is at a distance of 2.4$\pm$0.5~kpc (Parkes et al.
1980).

GX~304-1 was monitored with $EXOSAT$ covering a duration of an expected outburst
in 1984 July/August (Pietsch et al. 1986). However, no X-ray outburst was
detected during the $EXOSAT$ monitoring campaign. In contrast, the source
flux was estimated to be significantly low e.g. by a factor of 25, than the
quiescent flux level. This observed peculiarity was characterized as the X-ray
``off'' state of the pulsar. Long term optical monitoring of the Be companion
star in 1978-1988 suggested a major change (loss) in the Be envelop or circumstellar
disk, the consequence of which is considered as the possible cause of the X-ray
``off'' state in GX~304-1 (Corbet et al. 1986; Pietsch et al. 1986; Haefner 1988).

After 28 years of quiescence, an X-ray outburst was detected from GX~304-1 with the
{\it INTEGRAL} observatory in 2008 June (Manousakis et al. 2008) after which the source
was found to be active in X-rays. Since then, several X-ray outbursts have been detected
in the pulsar with {\it Swift}/BAT and $MAXI$ (Yamamoto et al. 2009, 2012; Krimm et al.
2010; Mihara et al. 2010). Using the {\it Rossi X-Ray Timing Explorer (RXTE)} observations
during 2010 August outburst, energy and luminosity dependence of pulse profiles were found
in GX~304-1 (Devasia et al. 2011). Apart from the evolution of pulse profiles, a
quasi-periodic oscillation (QPO) at $\sim$0.125~Hz was detected with harmonics in
several $RXTE$/PCA observations during this outburst. The pulsar spectrum in 3-30~keV
range was described with a partial covering high energy cutoff power-law
model (Devasia et al. 2011). During the same outburst in 2010 August, a cyclotron
absorption feature at $\sim$54~keV was detected in the pulsar spectrum (Yamamoto et al.
2011) and the corresponding magnetic field of the neutron star was estimated to be
$\sim$4.7$\times$10$^{12}$~G. A positive correlation between cyclotron energy and
luminosity was seen during 2012 January-February outburst with {\it INTEGRAL}
(Klochkov et al. 2012). Malacaria et al. (2015) performed timing and
spectral analysis of the pulsar using the same {\it INTEGRAL} data. The shape
of the pulse profiles obtained from these observations were found to be similar
in 20-40~keV, 40-60~keV and 18-80~keV energy ranges. Phase-resolved spectroscopy
was carried out by stacking multiple spectra of different fluxes. From this analysis,
the cyclotron absorption line energy was found to be nearly constant (within errors)
with pulse phases, except about 10\% variation at one phase bin (Malacaria et al.
2015). The evolution of the pulse period with luminosity was studied by using
data from $MAXI$/GSC, $RXTE$/PCA, $Swift$/XRT and $Fermi$/GBM observations
during a series of outbursts from 2009 to 2013 (Postnov et al. 2015; Sugizaki
et al. 2015). The observed pulse period variation was interpreted in terms of binary
modulation along with the spinning-up of the neutron star. The orbital parameters of
the binary system were estimated to be -- orbital period = 132.19~d, epoch at the
periastron = MJD~55425, pulse period $\simeq$275.45~s, orbital eccentricity
$\simeq$ 0.5, a$_x$ sin~$i$ $\simeq$ 500--600~light-s and  $\omega$ at periastron
$\simeq$ 122.5$^\circ$--130$^\circ$ (Sugizaki et al. 2015).

In this work, the timing and broad-band spectral properties of GX~304-1 were
presented in detail by using two {\it Suzaku} observations during its outbursts in
2010 August and 2012 January. Earlier, the evolution of pulse profiles up to
$\sim$30~keV had been reported by using $RXTE$/PCA observations during 2010
outburst (Devasia et al. 2011). Using {\it Suzaku} observations, the
evolution of pulse profiles up to $\sim$150~keV has been presented in this paper.
The observed changes in the shape of pulse profiles close to the cyclotron absorption
line are also being discussed. Although spectral studies of the pulsar during its 2012
outburst has been reported in 5-100~keV range by using {\it INTEGRAL} observations
(Malacaria et al. 2015), {\it Suzaku} observations provide a better opportunity to
investigate a detailed spectral and timing study in broad energy range (1-150 keV).
The details of observations, data analysis, results and interpretations are described
in following sections of the paper.

\begin{figure*}
\centering
\includegraphics[height=6.5in, width=4.6in, angle=-90]{fig3}
\caption{Energy-resolved pulse profiles of GX~304-1 obtained from XIS-0, HXD/PIN
and HXD/GSO light curves at various energy ranges, during second {\it Suzaku} observation
in 2012 January outburst. The presence of absorption dips in profiles at higher energies
can be seen at various pulse phases. The error bars represent 1$\sigma$ uncertainties.
Two pulses in each panel are shown for clarity.}
\label{erpp2012}
\end{figure*}

\section{Observation and Analysis}

{\it Suzaku}, the fifth Japanese X-ray mission, was launched by Japan Aerospace
Exploration Agency (JAXA) on 2005 July 10 (Mitsuda et al. 2007). It offers a
broad energy coverage (0.2-600~keV) in the electromagnetic spectrum by using
two sets of instruments e.g. the X-ray Imaging Spectrometers (XIS; Koyama et
al. 2007) and Hard X-ray Detectors (HXD; Takahashi et al. 2007). The XISs are
imaging CCD cameras and cover 0.2-12~keV energy range. Among four XISs, three
XISs (XIS-0, XIS-2, XIS-3) are front-illuminated whereas one XIS (XIS-1) is
back-illuminated. The effective areas of front and back-illuminated XISs are
340~cm$^2$ and 390~cm$^2$ at 1.5~keV, respectively. Field of view of XIS detectors
is $18'\times18'$ in full window mode. The HXD unit of {\it Suzaku} consists of two
sets of detectors such as HXD/PIN and HXD/GSO. HXD/PIN is a silicon diode detector
covering 10-70~keV energy range, whereas HXD/GSO is a crystal scintillator detector
working in 40-600~keV energy range.  Effective areas for HXD/PIN and HXD/GSO are
145 cm$^2$ at 15 keV and 315 cm$^2$ at 100 keV, respectively. Field of view of
HXD/PIN and HXD/GSO (up to 100~keV) is $34'\times34'$.

GX~304-1 was observed with {\it Suzaku} during its outbursts in 2010 August and
2012 January. $Swift$/BAT light curves of the pulsar in 15-50~keV range,
covering the outbursts are shown in top panels of Fig.~\ref{lc}.
Arrow marks in both panels indicate the date of {\it Suzaku} observation
of GX~304-1 during respective outbursts. During 2010 August outburst, the
{\it Suzaku} observation was carried out at the peak of outburst whereas the
second observation was made during the decay phase of the 2012 January
outburst. The first observation was performed on 2010 August 13, in
`HXD nominal' position with an effective exposure of $\sim$5.1~ks and
$\sim$12.9~ks for XIS and HXD detectors, respectively. However, the second
observation was made during 2012 January 31-February 02 for a longer effective
exposures of $\sim$16.5~ks for XIS and $\sim$58.7~ks for HXD. The
second observation was performed in `XIS nominal' position. During
both observations, the XIS detectors were operated in ``burst'' clock
mode with `1/4' window option yielding 0.5~s time resolution. The
publicly available archival data (observation~IDs: 905002010 and
406060010) were used in the present study. Heasoft software package
of version 6.12 and calibration database (CALDB) for XIS and HXD released
on 2014 February 03 and 2011 September 13, respectively, were used in
the data analysis.

The unfiltered event data files were reprocessed by applying the `aepipeline'
package of FTOOLS. The clean event files generated after the reprocessing of
XIS and HXD unfiltered event data were used in our analysis. The arrival times
of the X-ray photons recorded in XIS and HXD event data were corrected for solar
system barycenter by applying `aebarycen' task of {\small FTOOLS}. The light
curves and spectra of the pulsar were extracted from clean event data by using
the $XSELECT$ package of FTOOLS. The XIS event data were corrected for the effect
of thermal flexing and wobbling by applying attitude correction script
\textit{aeattcor.sl}\footnote{http://space.mit.edu/ASC/software/suzaku/aeattcor.sl}.
Subsequently, the pile-up estimation was made for XISs data by using S-lang script
\textit{pile\_estimate.sl}\footnote{http://space.mit.edu/ASC/software/suzaku/pile\_estimate.sl}.
For first observation, a pile-up of $\sim$22\%, $\sim$18\% and  $\sim$28\%
was found at the centers of XIS-0, XIS-1 and XIS-3, respectively. Therefore, an
annulus region with inner and outer radii of $60''$ and $180''$ was selected
to reduce the effect of pile-up to $\le$4\%. During the second observation,
the pile-up was estimated to be 17\%, 13\% and 18\% at the centers of XIS-0,
XIS-1 and XIS-3, respectively. An annular region with $40''$ inner and $180''$
outer radii was used to reduce the pile-up effect to $\le$4\% for the second
observation. These annulus regions were used for the extraction of source
light curves and spectra from cleaned XIS event data. The XIS background light
curves and spectra were extracted from the event data by selecting a circular
region away from the source. Response matrices and effective area files for
XISs were created by using `xisrmfgen' and `xissimarfgen' tasks of FTOOLS,
respectively. HXD being a non-imaging detector system, source light curves
and spectra were obtained from cleaned HXD/PIN and HXD/GSO event data by using
{\it XSELECT} package. However, PIN and GSO background light curves and spectra
were accumulated from simulated non-X-ray background event files provided by the
instrument team. A correction for cosmic X-ray background
(CXB\footnote{http://heasarc.nasa.gov/docs/suzaku/analysis/pin\_cxb.html})
was also applied to PIN spectrum. In our spectral analysis, HXD/PIN
response files released in 2010 July and 2011 June were used for 2010
August and 2012 January observations, respectively. For GSO data,
response and effective area files released in 2010 May were used for
2010 August observations.

\section{Results}

\subsection{Timing Analysis}

As described above, source and background light curves with 1~s time resolution
were extracted from barycentric corrected XIS-0, PIN and GSO event data for both
the observations. The $\chi^2$-maximization technique was used to estimate the pulse
period of the pulsar. Pulsations at periods of 275.45$\pm$0.05 and 274.88$\pm$0.01~s
were detected in the source light curves obtained from the first and second
{\it Suzaku} observations, respectively. Quoted errors in pulse period are
calculated for 90\% confidence level. The estimated pulse periods were used
to generate pulse profiles from background subtracted light curves from
corresponding observations. Pulse profiles in 0.5-10~keV (XIS-0), 10-70~keV
(PIN) and 40-200~keV (GSO) energy ranges for both the observations are shown
in second, third and fourth panels of Fig.~\ref{lc}, respectively.
Pulse profiles were generated by using 55421.7600 MJD as epoch (phase zero)
for the first observation where as 55957.4326 MJD was used for the second
observation.

Strong energy dependence of pulse profiles can be clearly seen during both
observations (Fig.~\ref{lc}) . Absorption dips at certain phases were seen
in the soft X-ray pulse profiles (0.5-10~keV range). However, these dips
disappeared from the pulse profiles in 10-70~keV range. The pulsations were
absent or marginally seen in 40-200~keV pulse profiles obtained from GSO
light curves. Apart from the energy dependence, the pulse profiles are also
found to be luminosity dependent. The top panels of the Fig.~\ref{lc} show
that the {\it Suzaku} observations of the pulsar were carried out at different
luminosity levels e.g. the source was comparatively brighter during the 2010
August observation than the 2012 January observation. However, the shape of
the pulse profiles in soft and hard X-rays (second and third panels) are
different due to the presence of absorption dips or dip-like features. Along
with the energy and luminosity dependence of the pulse profiles in GX~304-1,
a phase shift of $\sim$0.1 (see Fig.~\ref{lc}) was also found between the soft
(XIS) and hard (PIN) X-ray  pulse profiles obtained from both the observations.

To investigate the evolution of pulse profiles with energy during both
{\it Suzaku} observations, we generated energy resolved pulse profiles
in various energy bands and are shown in Fig.~\ref{erpp2010} \&
~\ref{erpp2012} for first and second observations, respectively. It
can be seen from Fig.~\ref{erpp2010} that a prominent and narrow
absorption dip was present in pulse profiles up to $\sim$8 keV. Beyond
this energy, the peak in the pulse profiles prior to the dip ($\leq$ 0.3
phase; left panels of Fig.~\ref{erpp2010}) disappeared and broadened
the minima in the pulse profile to 0.05-0.25 pulse phase range (panels
in second column of Fig.~\ref{erpp2010}). We suggest that this broadening
of the minima in the pulse profile is the possible cause of observed
$\sim$0.1 phase shift in the soft (0.5-10~keV) and hard X-ray (10-70~keV)
pulse profiles. A careful inspection of Fig.~\ref{erpp2010} \&
~\ref{erpp2012} showed that the pulse profiles were complex due to presence
of several absorption features (dips) at various pulse phases and strongly
energy dependent up to $\sim$12~keV beyond which the shape of the profiles
became simple up to $\sim$35~keV. The main dip in the pulse profiles
in this energy range (12-35 keV) was observed to be phase-shifted by
$\sim$0.1 phase compared to that in soft X-ray profiles. In pulse profiles
beyond $\sim$35 keV, the main dip at $\sim$0.1 phase appeared to be filled-up
gradually with increase in energy. Along with the increase in the normalized
intensity at $\sim$0.1 phase (Fig.~\ref{erpp2010} \& ~\ref{erpp2012}), a
significant decrease in intensity was observed at $\sim$0.7-0.8 phase range
which appeared as the main dip in hard X-ray pulse profiles. These hard X-ray
pulse profiles ($\geq$40~keV) appeared to be single-peaked and pulsations were
detected up to $\sim$120~keV.

\begin{figure}
\centering
\includegraphics[height=3.2in, width=2.4in, angle=-90]{fig4}
\caption{Energy spectrum of GX~304-1 in 1-130~keV energy range obtained with the XIS-0, XIS-3,
PIN and GSO detectors from the first {\it Suzaku} observation in 2010 August outburst,
along with the best-fit model comprising  a partial covering NPEX continuum model,
a Gaussian function for iron emission line and a cyclotron absorption component.
The middle and bottom panels show the contributions of the residuals to $\chi^{2}$
for each energy bin for the partial covering NPEX continuum model
without and with cyclotron component in the model, respectively.}
\label{spec2010}
\end{figure}

\begin{figure}
\centering
\includegraphics[height=3.2in, width=2.4in, angle=-90]{fig5}
\caption{Energy spectrum of GX~304-1 in 1-70~keV energy range obtained with the XIS-0, XIS-3 and PIN
detectors from the second {\it Suzaku} observation in 2012 January outburst, along with the
best-fit model comprising  a partial covering NPEX continuum model, a Gaussian
function for iron emission line and a cyclotron absorption component. The middle
and bottom panels show the contributions of the residuals to $\chi^{2}$
for each energy bin for the partial covering NPEX continuum model
without and with cyclotron component in the model, respectively.}
\label{spec2012}
\end{figure}

The energy resolved pulse profiles of GX~304-1 were found to be complex during
both the {\it Suzaku} observations. Presence of multiple narrow and prominent
absorption dips were seen up to as high as $\sim$50 keV. Beyond this energy,
the profiles appeared relatively simple. Presence of prominent dips up to higher
energies and sudden change in phase of main dip in pulse profiles beyond $\sim$35~keV
made it interesting to investigate the properties of pulsar through phase-averaged and
phase-resolved spectroscopy.

\begin{table*}
\centering
\caption{Best-fitting parameters (with 90\% errors) obtained from the spectral fitting of {\it Suzaku}
observations of GX~304-1 during 2010 August and 2012 January outbursts.
Model-1 : partial covering NPEX
model with Gaussian component; Model-2 : partial covering NPEX model
with Gaussian component and cyclotron absorption line.}
\begin{tabular}{lllll}
\hline
Parameter                      &  \multicolumn{2}{c}{2010 August}     	&   \multicolumn{2}{c}{2012 January}   \\
\\
                                &Model-1             &Model-2            &Model-1           &Model-2       \\
\hline
N$_{H1}$$^a$                    &1.04$\pm$0.02       &1.02$\pm$0.02      &0.98$\pm$0.02	    &0.97$\pm$0.02    \\
N$_{H2}$$^b$                    &13.2$\pm$1          &13.7$\pm$1.2       &5.7$\pm$0.5	      &5.3$\pm$0.5    \\
Cov. fraction                   &0.35$\pm$0.02       &0.32$\pm$0.02      &0.25$\pm$0.02	    &0.23$\pm$0.02	   \\
Photon index                    &0.6$\pm$0.03        &0.57$\pm$0.03       &0.42$\pm$0.02	    &0.43$\pm$0.02    \\
E$_{cut}$ (keV)	                &6.6$\pm$0.1         &7.1$\pm$0.2        &6.8$\pm$0.1       &7.4$\pm$0.2    \\

Fe line energy (keV)            &6.41$\pm$0.02       &6.41$\pm$0.02      &6.41$\pm$0.01     &6.41$\pm$0.01 \\
Eq. width of Fe line  (eV)      &44$\pm$7		         &43$\pm$8           &23$\pm$2          &23$\pm$3          \\

Cyclotron line energy (keV)     &--                  &53.2$\pm$0.8       &--                &50$\pm$1      \\
Width of cyclotron line (keV)   &--                  &6.5$^{+2.1}_{-1.6}$ &-- 	            &5.5$^{+2.6}_{-1.8}$   \\
Depth of cyclotron line	        &--                  &0.8$\pm$0.1        &--                &0.5$\pm$0.1 \\

Flux$^c$ (1-10 keV)             &9.2$\pm$0.5        &9.2$\pm$0.6        &4.9$\pm$0.2         &4.9$\pm$0.2 \\
Flux$^c$ (10-70 keV)            &24.5$\pm$1.5       &24.4$\pm$2.0        &9.6$\pm$0.5       &9.6$\pm$1.1   \\
Flux$^c$ (70-130 keV)           &0.2$\pm$0.1        &0.2$\pm$0.1         &--                &--           \\
$\chi^2$ (dofs)                 &857 (527)          &638 (524)           &863 (588)		     &765 (585)      \\
\hline
\end{tabular}
\\
\flushleft
$^a$ : Equivalent hydrogen column density in the source direction (in 10$^{22}$ atoms cm$^{-2}$ units),\\
$^b$ : Additional hydrogen column density (in 10$^{22}$ atoms cm$^{-2}$ units), \\
$^c$ : Absorption corrected flux in units of 10$^{-9}$  ergs cm$^{-2}$ s$^{-1}$.
\label{spec_par}
\end{table*}

\subsection{Spectral Analysis}

\subsubsection{Pulse-phase-averaged spectroscopy}

Phase-averaged spectroscopy was performed by using spectra accumulated from XIS-0,
XIS-1, XIS-3, PIN and GSO data obtained from both the observations. Earlier described
procedures were followed to obtain source and background spectra, response matrices
and effective area files for corresponding detectors. After appropriate background
subtraction, simultaneous spectral fitting was carried out by using {\small XSPEC}
v12.7 package. As the pulsar was bright during the first observation, broad-band
spectral fitting was carried out in 1-130~keV range. However, data in 1-70~keV
energy range were used for simultaneous fitting for second observation.
The XIS spectra from 2010 August observation were binned by a factor of 4 up
to 3~keV, a factor of 6 from 3 to 7~keV and a factor of 8 from 7 to 10~keV, whereas
for 2012 January observation, the XIS spectra were binned by a factor of 5 up to 10~keV.
PIN spectra from both the observations were binned by a factor of 2 from 25~keV to 45 keV,
a factor of 3 from 45~keV to 50 keV and a factor of 5 from 50 to 70~keV. The GSO spectra
were grouped as suggested by instrumentation team. Data in 1.7-1.9~keV and 2.2-2.4~keV
energy ranges were ignored from the spectral fitting due to the presence of known Si and
Au edge features in the XIS spectra. All the spectral parameters except the relative
normalization of detectors were tied together during the fitting.

\begin{figure*}
\begin{center}$
\begin{array}{ccc}
\includegraphics[height=5 cm,angle=-90]{fig6a.eps} &
\includegraphics[height=5 cm,angle=-90]{fig6b.eps} & \\
\includegraphics[height=5 cm,angle=-90]{fig6c.eps} &
\includegraphics[height=5 cm,angle=-90]{fig6d.eps} &
 \end{array}$
\end{center}
\caption{The $\chi^{2}$ confidence contours between high energy cutoff, cyclotron line energy and width,
obtained from the phase averaged spectra fitted by the partial covering NPEX model with cyclotron
component during 2010 August (upper panel) and 2012 January (lower panel) {\it Suzaku} observations.
The innermost to outermost contours represent 68$\%$, 90$\%$ and 99$\%$ confidence levels, respectively.
The ``+" sign indicates the best fit values for both parameters.}
\label{con-all}
\end{figure*}

It has been found that the phase-averaged spectra of Be/X-ray binary pulsars during
outbursts have been described by power-law (e.g. GX~304-1; Maurer et al. 1982), high
energy cutoff power-law (e.g. 4U~0115+63, 4U~1145-61, GX~304-1; White et al. 1983), Fermi
Dirac cutoff power-law (e.g. X0331+53, A~0535+26; Tanaka 1986), NPEX (e.g. 4U~0115+63,
X0331+53, Cep~X-4; Makishima et al. 1999) continuum models. However, recently it has
been found that while performing phase-resolved spectroscopy on data taken during X-ray
outbursts of these pulsars, above models do not yield acceptable fit at all phase bins,
specifically at phases of prominent and narrow absorption dips in the pulse profiles
(Naik et al. 2011; Paul \& Naik 2011; Naik et al. 2013 and references therein).
To investigate the changes in spectral parameters at all phase bins (dip and non-dip
phases of the pulse profiles), a partial covering absorption component has been added
to above standard continuum models. Addition of this component to the continuum model
resulted in getting acceptable fit to all phase bins and explained the cause of the
narrow and prominent dips in the pulse profiles. Partial covering absorption model
consists of two different power-law components with same photon index but different
normalizations, being absorbed by different column densities (N$_{H1}$ \& N$_{H2}$),
respectively (Endo et al. 2000).

In the beginning, standard continuum models such as high energy cutoff power-law
(HECUT; White et al. 1983), Fermi Dirac cutoff power-law (FDCUT; Tanaka 1986),
NewHcut (Burderi et al. 2000), cutoff power-law, NPEX (Makishima et al. 1999) and
Thermal Comptonization model (CompTT; Titarchuk 1994) were used in our spectral
fitting to describe the continuum spectrum of GX~304-1. Due to the presence of
narrow absorption dips in the pulse profiles of the pulsar (previous section) as
seen in other Be/X-ray binary pulsars, a partial covering absorption component
was added to above continuum models. Among these models, partial covering
NPEX continuum model was found to fit the source spectra obtained from both the
observations better than all other continuum models. We selected this model to use
in phase-averaged and phase-resolved spectral analysis of both the {\it Suzaku}
observations of GX~304-1.

The NPEX continuum model is a combination of two power-laws with positive
and negative indices and a high energy cutoff. This model is an approximation
of the unsaturated thermal Comptonization in  hot  plasma. The analytical form
of NPEX model is

\begin{eqnarray}
\centering
\nonumber
NPEX(E) = (N_1 E^{-\alpha_1} + N_2 E^{+\alpha_2})  ~ \exp \left( -\frac{E}{kT} \right)
\label{eq1}
\end{eqnarray}

where $N_1$, $\alpha_1$ and $N_2$, $\alpha_2$ are the normalization and photon index
of the negative and positive power laws, respectively. $kT$ represents the cutoff energy
in the unit of keV. The photon index of positive power law is fixed at a value of 2,
representing Wien's peak. During the spectral modeling, we found that the partial
covering NPEX model described the 1-130~keV (2010 observation) and 1-70~keV (2012
observation) spectra of the pulsar well. In addition to the continuum, iron fluorescence
emission line at $\sim$6.4~keV was detected in spectrum during both the observations. A
weak iron emission edge like feature was found in the residual during the fitting of
second observation. This was modeled by the addition of an edge component at $\sim$7.7~keV
in the spectral model.

An absorption like feature at $\sim$54~keV was clearly seen in residuals obtained
from spectral fittings of both the observations. Addition of a cyclotron absorption
component (`CYCLABS' in {\it XSPEC} package) in the partial covering NPEX
continuum model improved spectral fitting further with reduced $\chi^2$ of
$\sim$1.5 for both the observations. The values of reduced $\chi^2$, though acceptable,
are found to be large. Investigating the residuals in 1-10 keV range, we noticed a marginal
cross calibration uncertainties present between XIS-1 (back illuminated CCD) and XIS-0 \& 3
(front-illuminated CCD) spectra. While fitting the broad-band spectra without considering
data from XIS-1, the values of reduced $\chi^2$ obtained are 1.22 and 1.31 for first
and second observations, respectively. Best-fit model parameters obtained from
simultaneous spectral fitting of XIS-0 \& 3, PIN and GSO data are given in Table~1.
The energy spectra of the pulsar along with the best-fit model components are shown
in Fig.~\ref{spec2010} and ~\ref{spec2012}. The middle and bottom panels in each
figure show the residuals to the best-fit model without and with the addition of
cyclotron absorption feature in the continuum model, respectively. The $\chi^{2}$
confidence contours were plotted to check the dependence of the cyclotron line energy
on high energy cutoff and cyclotron width and are shown in the top and bottom panels
of Fig.~\ref{con-all} for first and second observations, respectively. We did not
find any strong degeneracy among these spectral parameters.

\begin{figure*}
 \centering
 \includegraphics[height=4.8in, width=3.9in, angle=-90]{fig7}
 \caption{Spectral parameters obtained from the phase-resolved spectroscopy
of GX~304-1 during the ${\it Suzaku}$ observation in 2010 August.
The first and second panels in both sides show pulse profiles of the pulsar
in 0.5-10~keV (XIS-0) and 10-70~keV (HXD/PIN) energy ranges. The values of
$N_{H_2}$, covering fraction, power-law photon index and cutoff energy
($E_{cut}$) are shown in third, fourth, fifth and sixth panels in left
side, respectively. The cyclotron line parameters such as depth (third panel),
line energy (fourth panel), source flux in 1-10 keV (fifth panel) and 10-70 keV
(sixth panel) are shown in right side of the figure. Solid circles in the fourth
panel in right side indicate that the cyclotron line energy was fixed for
corresponding phase-bin at the phase-averaged value. The errors in the figure
are estimated for 90\% confidence level.}
\label{sp2010}
 \end{figure*}

\begin{figure*}
\centering
\includegraphics[height=4.8in, width=3.9in, angle=-90]{fig8}
\caption{Spectral parameters obtained from the phase-resolved spectroscopy
of GX~304-1 during the ${\it Suzaku}$ observation in 2012 January.
The first and second panels in both sides show pulse profiles of the pulsar
in 0.5-10~keV (XIS-0) and 10-70~keV (HXD/PIN) energy ranges. The values of
$N_{H_2}$, covering fraction, photon index and cutoff energy ($E_{cut}$)
are shown in third, fourth, fifth and sixth panels in left side,
respectively. The cyclotron line parameters such as depth (third panel),
line energy (fourth panel), source flux in 1-10 keV (fifth panel) and 10-70 keV
(sixth panel) are shown in right side of the figure. The errors in the figure
are estimated for 90\% confidence level.}
\label{sp2012}
 \end{figure*}

\subsubsection{Pulse-phase-resolved spectroscopy}

Pulse profiles of GX~304-1 are found to be different even when compared
at same energy range from both {\it Suzaku} observations. Therefore,
it is interesting to perform phase-resolved spectroscopy to probe the changes
in spectral parameters with pulse phase and then compare
with the observations at different luminosity level. As the first
observation was for a relatively short exposure ($\sim$13 ks for HXD)
compared to the second observation ($\sim$59 ks for HXD), phase-resolved
spectroscopy was carried out by accumulating source spectra in 10 and 16
pulse-phase bins for first and second observations, respectively.
Reprocessed XIS and PIN event data from both the observations were used
to extract phase-resolved spectra by applying phase filter in $XSELECT$ package.
Data from HXD/GSO detector were not used in the phase resolved spectroscopy
due to lack of sufficient hard X-ray photons in each phase bin. Background
spectra and response matrices used in phase-averaged spectroscopy were also
used in phase-resolved spectral fitting. Simultaneous spectral fitting was
carried out on phase-resolved spectra obtained from both the observations
by using partial covering NPEX continuum model along with the cyclotron
absorption component and Gaussian function for the iron emission line.
While fitting, the values of relative instrument normalizations, equivalent
hydrogen column density (N$_{H_1}$) and iron emission line parameters were
fixed at the corresponding values obtained from phase-averaged spectroscopy.
The width of the cyclotron absorption line was fixed at the
phase averaged value to constrain the feature. Spectral parameters obtained
from fitting the XIS and PIN phase resolved spectra are shown in
Fig.~\ref{sp2010} and ~\ref{sp2012} for 2010 August 13 and 2012
January 31 observations, respectively. Pulse profiles obtained from
XIS-0 and PIN event data of each observation are also shown in top
two panels of these figures.

During both the observations, all the spectral parameters showed significant
variability with pulse-phase of the pulsar. Fig.~\ref{sp2010} (2010 August
observation) shows that the value of additional hydrogen column density
(N$_{H_2}$) varies in 1-30 $\times$ 10$^{22}$~cm$^{-2}$ range over pulse
phases. The value of N$_{H_2}$ was increased from 0.3 phase and became
maximum in 0.6-1.0 phase range. It can be seen that normalized intensity (XIS
pulse profile; top panel) was low at 0.6 phase and remain steady before reaching
the minimum value at 1.0 phase. Decrease in the normalized intensity of the pulsar
during above pulse phase range and simultaneous increase in the value of N$_{H_2}$
confirm that the plateau like feature in XIS pulse profile in 0.6-1.0 pulse phase
range was due to the presence of additional absorbing material close to the pulsar.
This can also explain the presence of an absorption dip in the XIS pulse profile
and an increase in the N$_{H_2}$ value in 0.3-0.4 phase range of the pulsar. As
in case of N$_{H_2}$, the covering fraction of the additional absorption was also
found to be comparatively high during the dip and plateau region. As expected,
the values of power-law photon index and cutoff energy were high
during the main dip in the XIS and PIN pulse profiles. The depth of the
cyclotron absorption feature was found to be variable and single peaked.
The energy of cyclotron absorption feature also showed variation over the
pulse phase of the pulsar. The values of both the parameters were maximum at
dip phase of the pulsar and gradually decreased to minimum value in 0.5-0.8
phase range. Data gaps in third and fourth panels in second column are due
to the non-detection of cyclotron features in the spectral fitting for
corresponding phase-bins. The flux in 1-10~keV and 10-70~keV shows
variation with pulse phase and follows the shape of pulse profile in respective
energy bands.

Though the shape of XIS and PIN pulse profiles of the pulsar were significantly
different during second {\it Suzaku} observation, the variation of spectral parameters
over pulse phase was comparable. High values of absorption column density
were found at phases of absorption dip in XIS pulse profile. The values of power-law
photon index, cutoff energy, depth and energy of cyclotron absorption line, source
flux in 1-10 keV and 10-70 keV were followed similar pattern as seen during
the 2010 August {\it Suzaku} observation of the pulsar. Though the number of absorption
dips and shape of the pulse profiles of the pulsar during both the observations were
different, presence of additional matter as the cause of absorption dips in the soft
X-ray profiles is supported by the findings in the present work. However, low value
($\le$5$\times$10$^{22}$ cm$^{-2}$) of absorption column density at $\sim$0.1-0.2 phase
range (Fig.~\ref{erpp2010} \& ~\ref{erpp2012}) suggested that the cause of absorption
dip at above phase range in the hard X-ray pulse profiles was different.

\section{Discussion and Conclusions}

Pulse profiles of transient X-ray binary pulsars are complex due to
the presence of multiple absorption dips/features at lower energies.
These absorption features are strongly energy dependent
-- prominent in soft X-ray pulse profiles and gradually disappear at
higher energies. Complex structures or absorption dips in pulse profiles
originate due to the photo-electric absorption of soft X-ray
photons by matter present around the neutron star. This can be confirmed
by investigating energy resolved pulse profiles and the evolution of spectral
properties with pulse phases of the pulsar. Among the accretion powered
X-ray pulsars, the pulse profiles of Be/X-ray binary pulsars during outbursts
are found to be complex. These pulsars show regular and periodic X-ray outbursts
(Type~I) that are associated with the periastron passage of the neutron star.
During periastron passage, the neutron star captures copious amount of matter
from the circumstellar disk of the Be companion star and undergoes X-ray
outbursts. Typical X-ray luminosity of the pulsar during Type~I outburst
is  $\sim$10$^{36-37}$~erg~s$^{-1}$ (Negueruela et al. 1998). In case of
GX~304-1, Type~I X-ray outbursts occur at a period of 132.5~d. Using
instruments with good time resolution and wide-band energy coverage
capabilities onboard {\it Suzaku}, we carried out a detailed study of
the pulsar during two Type~I outbursts. We also performed pulse-phase
resolved spectroscopy of GX~304-1 to study the evolution of spectral
parameters during these outbursts.

\subsection{Pulse Profiles}

Pulse profiles of GX~304-1 appeared to be different
during 2010 August and 2012 January Type~I outbursts.
During 2010 August observation, the profiles were complex due to the
presence/absence of peaks and dips at several pulse phases in soft and
hard X-ray energy ranges. Due to this, a phase shift of $\sim$0.1 was visible
between the soft and hard X-ray pulse profiles (Fig.~\ref{lc} \& ~\ref{erpp2010}).
However, the shape of the pulse profiles of the pulsar during 2012 January outburst
were significantly different compared to 2010 August outburst. Number of absorption
dips in the pulse profiles was more during 2012 observation. The strength of
these dips was also prominent compared to the earlier observation. These dips
were present in the pulse profiles up to higher energies unlike the 2010 August
observation, where the dips were seen in the pulse profiles up to $\sim$10 keV.
Pulse-phase resolved spectroscopy during both the observations revealed the
presence of additional matter at certain phases, causing the absorption dips
in the soft X-ray pulse profiles. During 2012 observation, more number of
narrow absorption dips in the pulse profiles suggest the presence of dense
narrow streams of matter around the neutron star. However, during 2010 observation,
relatively simpler profile with single absorption dip and a plateau phase suggests
that the matter distribution around the neutron star is different and relatively
simple. The luminosity of the pulsar during 2010 {\it Suzaku} observation was
estimated to be higher (2.3$\times$10$^{37}$ergs~s$^{-1}$) than the 2012
{\it Suzaku} observation (1$\times$10$^{37}$ergs~s$^{-1}$). The peak luminosity
of 2010 August outburst was also found to be high compare to the 2012 January
outburst (first panels of Fig.~1). As both the outbursts are Type~I X-ray outbursts,
observed difference in the shape of the pulse profiles must be due to the difference
in the subsequent mass accretion rate.

As in case of GX~304-1, another transient Be/X-ray binary pulsar EXO~2030+375
was also observed at the peaks of 2007 May and 2012 May Type-I outbursts with
{\it Suzaku}. The pulse profiles of EXO~2030+375 during these two outbursts were
significantly different (Naik et al. 2013; Naik \& Jaisawal 2015). During
the luminous outburst in 2007 May, the pulse profile of EXO~2030+375 consisted
of several absorption dips as seen in the pulse profiles of GX~304-1 during 2012
January outburst. However, during the less intense 2012 May outburst, the pulse
profiles were relatively smooth. Difference in the mass accretion rate during
these two Type~I outbursts was interpreted as the cause of different shape of
pulse profiles in EXO~2030+375. Such type of pulse profiles with multiple dips
are also seen in other Be/X-ray binary pulsars such as A0535+35 (Naik et al. 2008),
GRO~J1008-57 (Naik et al. 2011), 1A~1118--61 (Maitra et al. 2012 and references
therein). The dips in pulse profiles of these pulsars are originated due to the
absorption of emitted radiation by matter close to the neutron star. In most of
the cases, the dips in the pulse profiles are seen only in soft X-rays. However,
there are a few Be/X-ray pulsar in which the absorption dips are seen at same
phase in the pulse profiles up to higher energy ($\sim$70~keV) e.g. EXO~2030+375
(Naik et al. 2013). This is interpreted as due to the presence of dense additional
absorbers at various narrow pulse phase bins of the pulsar. Though, dip-like features
in GX~304-1 (present work) appeared up to $\sim$50~keV, the low value of additional
column density at dip phases suggests that absorption is not the cause of these
dips in hard X-ray pulse profiles.

Energy resolved pulse profiles of GX~304-1, obtained from both the {\it Suzaku}
observations revealed a significant phase-shift ($\sim$0.35) of the main dip in
profiles at energies below and above $\sim$35~keV. The observed phase-shift of
the main dip happened to occur at an energy close to the cyclotron absorption
line energy in GX~304-1. Such type of effects e.g. phase-shifts (lags) or
significant variations in pulse profiles close to the cyclotron absorption
line energy are also seen in two other Be/X-ray binary pulsars such as V~0332+53
(Tsygankov et al. 2006) and 4U~0115+63 (Ferrigno et al. 2011). Using a numerical
study on the effect of cyclotron resonant scattering in highly magnetized accretion
powered X-ray pulsars, Sch{\"o}nherr et al. (2014) showed that a strong change in
the pulse profile is expected at the cyclotron absorption line energy. This change
is attributed to the effects of angular redistribution of X-ray photons by cyclotron
resonant scattering in a strong magnetic field combined with relativistic effects.
In GX~304-1, we observed a significant change in the phase of main dip in the pulse
profile close to the cyclotron line energy. This detection, along with
the reported results from V~0332+53 and 4U~0115+63 supports the results obtained from
the numerical study of Sch{\"o}nherr et al. (2014).

\subsection{Spectroscopy}

Broad-band spectra of accretion powered X-ray pulsars are described by
several continuum models such as HIGHECUT, FDCUT, cutoff power-law, NPEX,
CompTT. Along with the continuum model, additional components such as
absorption due to matter present in the interstellar medium, blackbody/bremsstrahlung
for soft X-ray excess, Gaussian functions for emission lines and cyclotron resonance
scattering features (CRSF) are also needed to explain the observed spectrum. In
case of several Be/X-ray binary pulsars, a partially absorption component is being
used to describe the presence of several absorption features (dips) at certain phases
in the pulse profiles (Paul \& Naik 2011 and references therein). Detection of
CRSF in the broad-band pulsar spectrum provides direct estimation of
the magnetic field of X-ray pulsars. However, studies of CRSF at different pulse phases
of the pulsars can reveal important information about the magnetic field geometry around
the neutron star. Therefore, broad-band spectroscopy of data obtained from the
observations with high spectral capability instruments on-board {\it Suzaku}
is an appropriate tool to understand the properties of accretion powered X-ray pulsars.

This paper reports the broad-band phase-averaged and phase-resolved
spectroscopy of GX~304-1 by using two {\it Suzaku} observations during
its Type~I outbursts. The estimated values of galactic equivalent hydrogen
column density in the source direction (N$_{H_1}$) was same (within errors)
during both the observations. However, the values of additional column density
(N$_{H_2}$ - local to the pulsar), were found to be different during both
the observations. The value of N$_{H_2}$ was high during the 2010 August
observation compared to 2012 January observation. It should be noted here
that the luminosities of the pulsar during the {\it Suzaku} observation
(Table~1) as well as at the peak (top panels of Fig.~1) of 2010 August
outburst were high compared to corresponding values during 2012 January
outburst. This confirms that the amount of mass accreted by the neutron
star from the Be circumstellar disk during 2010 August outburst was
significantly more than that during 2012 January outburst. Similar findings
have also been reported for EXO~2030+275 during its Type~I outbursts with
significantly different luminosities (Naik et al. 2013; Naik \& Jaisawal
2015). High value of N$_{H_2}$ during more luminous Type~I outbursts in
Be/X-ray binary pulsars can be explained as due to significant amount of
mass accreted by the neutron star from the circumstellar disk of the Be
companion star.

We estimated the effect of additional column density (N$_{H_2}$) on the phase
averaged spectrum by taking the difference in absorption corrected flux without and
with N$_{H_2}$ component. It was found that the 2010 August observation was more
affected by absorption due to additional matter compared to the 2012 January
observation. The flux differences were estimated to be (1.8$\pm$0.9$)\times$10$^{-9}$
and (0.4$\pm$0.3$)\times$10$^{-9}$ ergs~cm$^{-2}$~s$^{-1}$ for 2010 August and 2012
January observations, respectively. The covering fraction which is defined as
{\it Norm2/(Norm1+Norm2)}, where $Norm1$ and $Norm2$ are the normalizations of
first and second power-law, was also found to be high during first observation.
Covering fraction describes the possibility of interaction of photons with
the absorbing matter which is marginally offset from the line of sight at a phase
averaged solid angle of {\it $\Omega$/4$\pi$= Norm2/Norm1} (Endo et al. 2000). The
averaged phase solid angles ($\Omega$/4$\pi$) for first and second observations were
estimated to be 0.47 and 0.30, respectively. This indicates that the additional
absorbing matter during first observation was present relatively more closer
to the neutron star that extending to a larger solid angle.

Absorption dips in the pulse profiles of Be/X-ray binary pulsars are explained
as due to the presence of narrow streams of matter that are phase-locked with the
neutron star. The magnetospheric radius of the pulsar can be used to constrain the
location of additional absorbing matter in such narrow streams. The size of
magnetosphere of the pulsar depends on the mass accretion rate and the strength
of the magnetic field (Mushtukov et al. 2015a and references therein) through the
relation
\begin{equation}
R_{\rm m}=2.6\times 10^8
 M^{1/7}R_6^{10/7}B_{12}^{4/7}L_{37}^{-2/7} \ \mbox{cm}
\end{equation}
Using standard values of mass and radius of canonical neutron stars and the observed
luminosities of GX~304-1 in above equation, the magnetospheric radii were estimated
to be $\sim$5100 and 6300~km during first and second observations, respectively.
This confirmed that the pulsar magnetosphere was relatively small during the first
observation. Therefore, the streams of additional matter were present within the
magnetosphere and found to be closer to the pulsar during the first {\it Suzaku}
observation.

Pulse-phase resolved spectroscopy of GX~304-1 during two Type~I outbursts
showed the presence of narrow streams of matter (higher value of N$_{H_2}$) at
several pulse phase ranges. The presence of such streams of matter are interpreted
as the cause of absorption dips detected in soft X-ray pulse profiles of the pulsar.
Several such dips are seen in the pulse profiles of Be/X-ray binary pulsars during
X-ray outbursts. Density and opacity of matter in these narrow streams decides the
energy dependence of the dips in the pulse profiles of these pulsars. During both
the observations, pulse-phase variation of covering fraction was found to be similar.
We suggest that the geometry or distribution of absorbing matter around the pulsar
is probably similar during both observations but at different locations.

\subsection{Cyclotron line in GX~304-1}

Cyclotron absorption line or CRSF was clearly detected in the
spectra of GX~304-1 during both the observations and was described
with pseudo-Lorentzian function (CYCLABS) in the continuum model.
These are absorption like features which appear in hard X-ray spectrum
($\sim$10-100~keV) through the resonant scattering of the photons with
electrons in strong magnetic field ($\sim$10$^{12}$~G) near the poles of
the neutron star. The cyclotron line energy is related with the magnetic
field through the relation {\it E$_{cyc}$=11.6B$_{12}\times(1+z){^{-1}}$
(keV)} or 12-B-12 rule, where B$_{12}$ is the magnetic field in the unit
of 10$^{12}$~G and $z$ is the gravitational red-shift. Detection of
CRSF in the pulsar spectrum, therefore, provides  the direct measurement
of the magnetic field of the neutron star. Though, CRSF was already detected
in GX~304-1 (Yamamoto et al. 2011), {\it Suzaku} observations
at different source intensities provide an opportunity to
investigate the luminosity dependence of the cyclotron line energy.
The cyclotron feature was detected at $\sim$53 and 50~keV during 2010 August
and 2012 January {\it Suzaku} observations, respectively. The observed
cyclotron absorption line energies are not significantly different.
However, it shows a positive dependence on the pulsar luminosity, as seen
in Her~X-1 (Staubert et al. 2007). In some other cases such as 4U~0115+63
(Nakajima et al. 2006; Tsygankov et al. 2007), and V~0332+53 (Tsygankov et al.
2010), a negative correlation is observed between the luminosity of pulsar
and the cyclotron absorption line energy.

Attempts have been made to explain the observed positive and negative
correlation between pulsar luminosity and the cyclotron line
energy. A negative correlation is expected in super-critical regime
where the source luminosity is higher than the critical luminosity
(Becker et al. 2012; Mushtukov et al. 2015a). Above critical luminosity,
density of infalling matter becomes so high that the particles start
interacting and decelerating through the formation of a radiation-pressure
dominated shock above the neutron star surface. Cyclotron scattering features
most likely occur closer to the shock region. With increasing luminosity, the
shock height drift upwards in the accretion column where relatively low
strength of magnetic field produces cyclotron feature at lower energy. It
explains negative correlation as observed in 4U~0115+63 and V~0332+53. However,
the positive correlation is predicated for a sub-critical regime e.g. below
critical luminosity. The pressure of accreting matter in this regime pushes
hydrodynamical shock closer to the neutron star surface where increase in
the strength of magnetic field with luminosity results a positive correlation
between the cyclotron line energy and luminosity (Staubert et al. 2007), as seen
in Her~X-1 and GX~304-1. The 1-70 keV luminosity of GX~304-1 during first and
second {\it Suzaku} observations was estimated to be 2.3$\times$10$^{37}$
and 1$\times$10$^{37}$ergs~s$^{-1}$, respectively, which lies in the sub-critical
regime (Mushtukov et al. 2015a) and expected to show a positive correlation
 with cyclotron line energy.

Poutanen et al. (2013) and Nishimura (2014) have proposed alternate models
to describe the dependence of cyclotron absorption line energy on the source
luminosity. In these models, it is argued that the formation of cyclotron line
in direct spectrum is questionable due to the large gradient of magnetic field
strength along line forming region in the accretion column. However, cyclotron
line (CRSF) can be formed in the reflected radiation from the surface of the
neutron star where magnetic field gradient is relatively small (Poutanen et al.
2013). It is widely believed that the accretion column height is linearly
dependent on source luminosity ($>$10$^{37}$~ergs~s$^{-1}$) or accretion rate.
At higher luminosity, larger area on neutron star surface (from the poles with
strong magnetic field towards equator with weak field strength) is expected to
be illuminated for cyclotron interactions. This explains the observed
anti-correlation between cyclotron line energy and luminosity, as seen in
V~0332+53. However, Nishimura (2014) described the observed correlations by
considering the changes in polar emission region, direction of photon
propagation and the shock height. The negative correlation was interpreted
in terms of shock region displacement whereas the positive correlation was
explained by using the changes in beam pattern. In case of GX~304-1 (present
work), the cyclotron absorption line width, depth and ratio of line width and
energy (W/E$_{cyl}$) show positive correlation with luminosity. The observed
positive correlation between the cyclotron line energy and luminosity in
GX~304-1, therefore, can be explained as due to the change in beam pattern,
as described by Nishimura (2014). Alternatively, Mushtukov et al. (2015b)
discussed the positive luminosity dependence of sub-critical X-ray pulsars
like GX~304-1 by studying the changes of plasma velocity profile in line-forming
region under influence of radiation pressure from the hot-spot. The cyclotron line
energy at a luminosity was determined by corresponding redshift from
velocity profile at a given height. This model successfully predicts
the positive luminosity correlation of cyclotron line energy for pulsars
like GX~304-1 along with cyclotron line width dependence on luminosity and
pulse phase variation of cyclotron line parameters, which were not being
discussed in Nishimura (2014).

Investigation of the change in cyclotron parameters with pulse phase
of the pulsar provides important evidences to understand the emission
geometry as well as the magnetic field mapping around the neutron star.
A comparative study of these parameters at different intensity levels
during several outbursts can also yield information about the changes
in emission or accretion column geometry. Pulse-phase resolved spectroscopy
of cyclotron absorption line is one of the interesting results of this work.
During both {\it Suzaku} observations of the pulsar, cyclotron energy and depth
were found significantly variable with pulse-phase. Change in cyclotron
line parameters with pulse phase has also been seen in other X-ray pulsars such
as Cen~X-3 (Burderi et al. 2000), GX~301-2 (Kreykenbohm et al. 2004), 1A~1118-61
(Maitra et al. 2012), A~0535+26, XTE~J1946+274, 4U~1907+09 (Maitra \& Paul 2013),
V~0332+53 (Lutovinov et al. 2015) and Cep~X-4 (Jaisawal \& Naik 2015) with
$\sim$10-30\%  variation in cyclotron energy.

The cyclotron line energy for GX~304-1 was found variable with phase up
to 17\% and 24\% for first and second {\it Suzaku} observations, respectively.
However, the cyclotron line depth showed phase dependence within a factor of
$\sim$2.5 for both observations. Various simulations were performed to study the
dependence of the cyclotron line on pulsar phases, assuming certain sets of
rule and geometry in line forming region (Sch{\"o}nherr et al. 2007; Mukherjee
\& Bhattacharya 2012). These studies predicated that 10-30\% variation
in cyclotron energy with phases can be resulted due to effects of viewing angle
of accretion column or emission region. However, more than 30\% changes in
cyclotron energy is contributed by distortion in the magnetic field geometry.
In GX~304-1 (present work), cyclotron energy is found to be variable within
24\% for both observations which can be explained as effects of viewing angle
or local distortion in the magnetic field in line forming region. We found that
the cyclotron energy and depth for both observations were peaking around the 1.0-1.1
(or 0.0-0.1) phase range, which lies closer to the peak of pulse profiles at
$\geq$35~keV. This result supports the effect of cyclotron resonance
scattering on beaming pattern that changes the shape of the pulse profiles.

In summary, the timing and spectral properties of GX~304-1 were presented by using
{\it Suzaku} observations during Type~I outbursts. Absorption dips were detected in the
pulse profiles at soft X-rays. These dips were originated due to obscuration/absorption
of X-ray photons with narrow streams of accretion flow at certain pulsar phases.
The shape of pulse profiles was significantly changed at $\geq$35~keV e.g. close
to the cyclotron line energy. Significant pulse phase dependence of cyclotron line
was explained as the effects of viewing angle or the role of complicated magnetic
 field of the pulsar.

\section*{Acknowledgments}

We sincerely thank the referee for his/her valuable comments and suggestions which
improved the paper significantly. The research work at Physical Research Laboratory
is funded by the Department of Space, Government of India. The authors would like to
thank all the members of the Suzaku for their contributions in the instrument
preparation, spacecraft operation, software development, and in-orbit instrumental
calibration. This research has made use of data obtained through HEASARC Online
Service, provided by the NASA/GSFC, in support of NASA High Energy Astrophysics
Programs.

redpajama_set_name: RedPajamaArXiv


text:
Benjamin Johannes "Ben" Viljoen (7 September 1869 – 14 January 1917) was an Afrikaner-American Consul, soldier, farmer, Maderista, and Boer general. Viljoen was born in a cave in the Wodehouse district of the Cape Colony to Susanna Magdalena Storm and Wynand Johannes Viljoen. This was the temporary residence of the Viljoen family while their farm house was being constructed. He spent his early years on the Varkiesdraai farm near Umtata. He attained the position of Assistant Commandant-General of the Transvaal Burgher Forces and was member for Krugersdorp in the Transvaal Volksraad. He was a South African Freemason.

Krugersdorpse Vrywilligerskorps and the Volksraad
In 1890 he moved to Johannesburg and in 1896 he founded the Krugersdorpse Vrywilligerskorps experiencing combat with the Jameson Raiders. On the Uitlander issue, Viljoen was an ally of Paul Kruger. He is famously attributed to saying in the Volksraad that it was time to put trust in "God and the Mauser".

Outbreak of War
With the outbreak of the Second Anglo-Boer War he first did service in the Colony of Natal. He led the Johannesburg Commando, the great nemesis of the Uitlanders and he fought at the Battle of Elandslaagte on 21 October 1899. When the front disintegrated, he joined up with other Boers to stop the British march on Pretoria.

When British General Ian Standish Monteith Hamilton crossed the Vaal River on 26 May 1900, Viljoen and his Johannesburg Commando confronted him with De la Rey and the Lichtenburg Commando.

Guerrilla war
With the end of the conventional phase of the war, he formed a powerful guerrilla commando consisting of men from Johannesburg, Krugersdorp, Boksburg and the North and East Transvaal. His success resulted in him attaining the high rank of Assistant Commandant-General (November 1900). Viljoen's exploits included surprising a garrison at Helvetia in the Eastern Transvaal on 29 December 1900 and temporarily capturing 235 men and a 4.7-inch gun.

Capture, imprisonment and war memoirs
He was eventually captured at Lydenburg on 25 January 1902 and remained prisoner-of-war until May 1902 at the Broadbottom Camp, on St. Helena. It was there that he wrote his autobiography, "My Reminiscences of the Anglo-Boer War". The book is a realistic description of the war from a Boer perspective. Unlike other Boer generals he was not a property owner and thus hesitated to return to South Africa. He returned to South Africa as a pauper but refused to take British citizenship, thus greatly reducing his chances of resuming a public career. He was also disillusioned by rumours claiming that he had collaborated with the British, and he felt that his contribution to the struggle was not recognised.

Boer Colony in Mexico
Ben Viljoen was one of the South African refugee officers who formed a farm colony in Mexico with the assistance of Theodore Roosevelt. Help with selecting and negotiating for the property were provided by two men hired by Roosevelt family friend Marshall Latham Bond and the husband of a Roosevelt relative Edward Reeve Merritt. It was located at Hacienda Humboldt in the municipality of Julimes, Chihuahua.

United States and the Boer War Circus
He left for the United States in 1904 along with General Piet Cronjé (of Battle of Paardeberg fame) to take part in the Louisiana Purchase Exposition (St. Louis, Missouri) and the so-called "Boer War Circus" – portrayals of scenes from the Boer War. After leaving the fair, he settled down in the US. He divorced his wife, Lenie (née Els), who did not really want to leave South Africa, when the news reported he was engaged to May Belfort. He later married a US woman, Myrtle Dickerson. Attempts to establish a Boer settlement in the north of Mexico ended in failure.

Civic life in New Mexico
He returned from Mexico to the US and was instrumental in organising Boer colonies in Doña Ana County at Berino, Chamberino and La Mesa in New Mexico Territory. He became involved in civic affairs throughout the Mesilla Valley, and in 1909 he was granted US citizenship. Viljoen became familiar with both President Theodore Roosevelt and New Mexico Governor George Curry. Viljoen was commissioned as a Major in the territorial National Guard's First Regiment of Infantry. In 1911, he travelled to Washington, D.C., with Curry and Albert Bacon Fall as part of a delegation promoting statehood for New Mexico. In April and May 1911, he fought with the Mexican Revolutionary Francisco Madero at the Battle of Ciudad Juarez.

Viljoen was also influential in agriculture. He introduced new crops and farming practices to the Mesilla Valley. Viljoen was interested in the creation of the Elephant Butte Dam and developed irrigation systems for the valley.

For a short while, he was US Consul in Germany, and also acted as military advisor to Francisco Madero until Madero's assassination in 1913. He died in 1917, at his farm in La Mesa and is buried at the Masonic Cemetery in La Mesa, New Mexico.

Notes

External links

1869 births
1917 deaths
People from the Eastern Cape
Afrikaner people
Members of the Dutch Reformed Church in South Africa
South African people of Dutch descent
South African Republic generals
History of New Mexico
South African expatriates in Mexico
South African diaspora
South African prisoners of war
South African writers
South African Republic military personnel of the Second Boer War
Members of the Volksraad of the South African Republic
South African emigrants to the United States
People of the Mexican Revolution
 South African Freemasons

redpajama_set_name: RedPajamaWikipedia


Construction at 1830 Sutter St. on Aug. 12 (above) and April 1 (below).
SAN FRANCISCO — Nihonmachi Little Friends' (NLF) new preschool building on Sutter Street in Japantown is well under way with the full framework nearing completion.
Concrete has been poured on all levels, including the rooftop, which will be a play area and children's garden for science and nature studies. Scaffolding has been erected on the west side of the building to install the siding.
NLF's Plant a Seed Campaign (PASC) project was launched in 2012 to build a preschool addition to its historic 1830 Sutter St. facility, on its adjacent playground lot.
Once a single preschool with 15 children, NLF has grown into a premier childcare center with three sites, serving over 200 children annually with ages ranging from 2½ to 12 years. Over 3,000 children have attended NLF since it was founded in 1975. Its award-winning Japanese bilingual and multicultural programs attract a broad range of families from diverse ethnic and economic backgrounds.
Fundraising for the new building addition is continuing during the construction period, with two events planned for this fall: the Big Steps for Little Friends 5K Run/Walk on Sunday, Oct. 9, in Golden Gate Park; and the Sushi Social/41st Anniversary of the agency at its Sutter building on Friday, Nov. 18. Naming opportunities are still available starting at $1,000, with recognition on donor boards in the new building lobby.
Information on all of these ways to help NLF reach its goal can be found at its website, www.nlfchildcare.org.


The SCHAUFLER Academy, the international training centre of BITZER, launched the event management software EMS in autumn 2017.
After almost a year in use, we asked Volker Stamer (Director SCHAUFLER Academy) about his experience with the software so far and how it can be used.
BITZER: Mr Stamer, how did the idea come about to launch the BITZER event management software EMS?
Volker Stamer: Ever since the SCHAUFLER Academy opened in February 2016, the number of our events and their participants has grown rapidly. Whereas there were 2,300 participants in the first year, that number had increased to 4,300 by the second year. In order to meet the increasing requirements, we continuously test the efficiency and effectiveness of our processes. We concluded that some processes had to be automated to an even greater extent in order to provide customers with an even easier way to access information about our events.
Ultimately, a decision was made in favour of BITZER EMS, an event management software which guarantees our customers maximum flexibility. In this context, flexibility means that they are able to plan their events based on their individual wishes and expectations. Led by Angela Müller, who served as the project manager, a total of 12 BITZER employees from eight departments were involved in the development of the tool. It took around one year to complete BITZER EMS.
BITZER: How long have you had BITZER EMS?
V.S.: The first event to be organised using BITZER EMS was 'Quo Vadis' in October of last year. All events at the SCHAUFLER Academy have been running through our event management software since then.
BITZER: How can prospective participants find the page?
V.S.: You can either click on SCHAUFLER Academy Training and Seminars under 'Service' on the BITZER website or type in www.trainings-events.bitzer.de. This page contains an overview of all our events including a current agenda, price overview, participant limits, a registration tool and information about the event location, the hotel and the surrounding area. This way, prospective participants have all relevant information at their fingertips and can be sure that it is always up to date.
BITZER: What are the features and benefits of the software? Who is it designed for?
V.S.: For one, the event software is designed for the organisers at the SCHAUFLER Academy who use the tool to manage content and participants. Additionally, it provides a simple platform for all training course attendees and event participants to access information about and register for events in the SCHAUFLER Academy. Regardless of who is planning the event, customers are always provided with the same quality. All of our events undergo the same process with BITZER EMS, which means that they have the same structure and appearance. The software is currently available in two languages, German and English, built into a responsive design.
The SCHAUFLER Academy has taken a hands-on approach from the outset, which is reflected in our training courses and now also in the event software. Every participant can be certain that our Academy focuses not on teacher-centred learning, but rather on practical applications and sample products. Participants work in a hands-on manner, helping them to learn as successfully as possible. Yet the SCHAUFLER Academy is not only open to training course attendees, but also all other customers such as partners, suppliers and associations. They can book the rooms of the SCHAUFLER Academy for their own events, which means we also act as a service provider. Our training courses and events are complemented by an attractive general programme such as punting in Tübingen or Segway tours in the Black Forest. BITZER EMS takes all individual requests into account, which is why we often say that the software leaves no wish unfulfilled.
BITZER: Do the numerous possible selections also pose a challenge for the user?
V.S.: As with any software, BITZER EMS has a learning curve. The transition did not take place overnight, but rather was a weeks-long process comprising many training courses. For the project team, it was important that all training organisers at the SCHAUFLER Academy were able to get the most out of the event software. As it is so flexible and responds to all customer preferences, BITZER EMS requires a high degree of expertise which we have built up since last year.
Customers, however, do not have to familiarise themselves – they enjoy all of the benefits of the event software from the first event. Where necessary, our automated registration process encloses visa letters and asks about individual requirements such as dietary preferences or the level of knowledge of the participants. Links, videos and group pictures can be added to the software and sent to all participants at the click of a button. Even after the event, BITZER EMS remains a powerful tool, as digital feedback questionnaires can be integrated into it and evaluated automatically.
BITZER: Are there plans for the future?
V.S.: BITZER EMS is a global solution that can be used for the entire company and all subsidiaries. The objective is to provide all BITZER customers with a uniform, improved service, regardless of the event in which they are participating. The software makes it possible to rule out errors and present the same appearance and the same process internationally. Naturally, adjustments have to be made for subsidiaries, for example, yet the uniform appearance does not change. We at the SCHAUFLER Academy see BITZER EMS as a constantly growing catalogue that can be adapted. This fits in with our fast-moving world in which we have to respond to customer requests promptly and continuously. With regard to customer requests, we are happy to receive them not only through our website, but also by email . We look forward to hearing your opinions!