On my return to IBE this time around it became another memorable moment in my life. It has become a true hip hop/bboy festival! So many bboys and bgirls in attendance it is something to experience. It was very nice meeting so many people this last weekend. I was running around with the Red Bull BC one all stars as well as Squadron members. So much to do and so many categories to watch i just roamed around and caught whatever I could. I sat through a few panels which I thiught were well done. On Saturday Ronnie and myself had a talk show about our bboy careers and just on our beliefes as bboys and our approaches. I was flatered to be a part of this. We went through many subjects from our back grounds to our battle approach. The two subjects that i really enjoyed talking about, One was music and the other was the internet age of bboyn. We ended up getting a good turn out considering all the battles that were happening at the same time. I want to say thank you to those that came out. They had some good questions. Ill try and cover these later.
Then came the day of the all battles all which had a new concept as far as teams. It was great to be apart of The notorious team. When they announced me i was surprised at the response i received. A lot of love! Made me feel more comfortable for the battles. The energy we had in the first battle between the Legends and us was incredible. So much hype it is hard to put it in words! wow!! I also enjoyed battling the Present Players mad respect and straight battle. They did well I wish they would gave us a little more time to rest in between. Still dope though. Overall a fun trip once again to the IBE! Happy 10th yr anniversary. I hope it doesnt take me 5 more years to go back. Heres some pics of the trip.


The Croft. Self Catering Holiday Cottage in Tobermory.
Situated in upper Tobermory, the Croft is a very spacious Mull holiday house in a great location with excellent views over Tobermory and the sea. This is a well-appointed property furnished to a very high standard, making a brilliant base for family holidays or group getaways. Socialise on the sun deck with sea views, cosy up in the living room or cook up a feast in the kitchen – there's plenty of room for the whole family here.
There is parking outside for two cars and the entrance leads to the hall and stairway. The modern, spacious and bright kitchen is well-equipped and has a large window at one end. Double glass doors at the other end lead onto the veranda, letting lots of natural light pour in and showcasing the views outside. The dining table is part of the open plan area off the kitchen. On a sunny day, guests will enjoy opening the doors to the veranda to create a sense of semi outdoor dining.
The main living area is spacious with high quality, comfortable furnishings, a good selection of books and interesting reading material about the island. There is plenty of seating and double doors lead directly into the sunroom, which, if you can stop yourself from looking at the view, is a great place to read a book or catch up with emails (wireless internet access is provided).
From the main living room a corridor runs to the downstairs double bedroom, bathroom and optional spare bedroom with a handy fold out sofa bed. The owners of this self-catering cottage are hoteliers, and they have used their expertise in this area when furnishing and appointing the property. As a result, all of the beds and linen are of an excellent quality and comfort, giving you hotel luxuries in the home-from-home environment of this excellent holiday cottage.
The upstairs bedroom is a large spacious room, with plenty of storage space and views to the sea. The twin room upstairs is equally large and has a window looking out onto the hills behind The Croft. There is also a good-sized bathroom upstairs with a very large shower. This is a warm well insulated property, and makes for a very comfortable, relaxing house to holiday in.
There are some lovely walks straight from the door. Turning left a short walk up onto the open hill tops rewards with a fantastic panoramic view, particularly impressive is the view of Ardnamurchan peninsular and out to the Atlantic Ocean beyond. A 10-minute walk down the hill from The Croft will take you to Tobermory's main street, right on the harbour front. Here you will find many good eateries, shops, cafes and pubs along with some lovely coastal walks to explore too.
The Croft has a small planted garden by the front door, and a larger hill garden to the rear, where there is a large veranda with excellent views, a seating area for dining outside, and two entrances into the house, one into the sunroom, another via double doors into the dining room. It offers a picturesque, peaceful holiday home on the doorstep of the island's charming capital – the best of both worlds!
Living Room: Large family lounge with comfortable seating, television (freesat channels) and feature fire.
Kitchen and Dining Area: Fully fitted kitchen with cooker, hob, fridge, freezer, microwave, dishwasher, washing machine and dryer. Dining area with table seating eight.
Sun Lounge: With direct access to terrace and garden area.
Bedrooms: Ground floor double bedroom (king size) and further bedroom with foldaway double. An additional double bedroom (king size) and one twin bedroom on the first floor.
Bathrooms: Ground floor bathroom and first floor bathroom (both with basin, w.c, bath and separate shower unit).
More at this Property: Wireless internet access. Cot and high chair can be provided on request. Discounts for dining at Highland Cottage restaurant in Breadalbane Street.


This first ATC is one I did for the February Winner-Take-All Swap on Paper Traders. It was won by Lucy.
I made these Peeled Paint ATCs for Letha's Way Out West swap.
These little Bird Book Pages were made for my Bird Deco Swap.
Most have been traded but I did get to keep two of them. Birds are a favorite theme of mine and I am thrilled with how they turned out ... and with all the lovely pages I got in the swap. One day they will all be assembled into a little book with some other birdie pages that I am working on.
This final picture is of my page for the PT Counting Crows swap.


text:
Home Bollywoood Updates Here are all the details about Ranveer Singh's character in Padmavati
Here are all the details about Ranveer Singh's character in Padmavati
Here are all the details about Ranveer Singh's character in Padmavati
Sanjay Leela Bhansali next magnum opus is much talked about already and here are all the details about Ranveer Singh's character in Padmavati.
Padmavati is going to be based on Rani Padmavati, about Sultan Alauddin Khilji and his obsessive love for Queen of Mewar Padmavati. Khilji's role will be played by Ranveer Singh while Deepika Padukone will play the queen and we bring to you all the details about Ranveer Singh's character in Padmavati.
This is going to be the first time Sanjay Leela Bhansali is treading into these waters and making a movie on the 'antihero'. Sanjay has always loved this all-destructive romantic tale. Alauddin was a genius who was shrewd and ambitious. He was absolutely smitten by Rani Padmini's bewitching beauty and unmatchable intellect. This film will be about the queen's courage to fight her undefeated nemesis.
According to a source of koimoi, "Ranveer Singh essays the role of the larger-than-life Alauddin Khilji in Padmavati. He has been very excited about it ever since he signed the film. Alauddin Khilji is a character that Sanjay Leela Bhansali wanted to bring to life onscreen since a long time."
Shahid Kapoor will be seen playing the Chittor King who is married to Rani Padmavati of Chittorgarh. How excited are you about the movie?
Kabir Singh Becomes first 'A' rated Bollywood film to cross 200 crore mark
Kabir Singh beats Kesari and Total Dhamaal, becomes 3rd highest grosser of 2019
Kabir Singh 4th Day Box Office Collection: Shahid Kapoor's Film Is Unstoppable
Highest Grossing Movies Of Shahid Kapoor, Kabir Singh Tops The List
Kabir Singh 1st Day Box Office Collection: Fourth Highest Opening Of 2019
Actors With Most Movies In 100 Crore Club: 100 Crore Movies Of Bollywood Actors
4 Best Male Dancers Of Bollywood, Vote For The Best Now
Ranveer Singh's Top 10 Opening Day Grossers: Simmba Tops The List
Gully Boy 1st Day Box Office Collection: Ranveer Singh's Film Is Off To A Huge Opening
Bollywood 200 Crore Club Movies, Facts And Detailed Report
Tamasha Box Office Collection and Verdict depend on these factors
IPL 2016 Opening Ceremony is going to be a Star-Studded Event
Another Catfight Begins as Sonakshi Criticizes Deepika's Video

redpajama_set_name: RedPajamaCommonCrawl


text:
Xan Fredericks
National Map Liaison FL, PR, USVI
NGP User Engagement Office
afredericks@usgs.gov
2639 N Monroe St # 200A
3DEP
Xan works with the National Geospatial Program as the National Map Liaison to Florida, Puerto Rico, and the U.S. Virgin Islands and is a Geospatial Information Response Team Operations Officer.
Alexandra "Xan" Fredericks is the National Map Liaison to Florida, Puerto Rico, and the U.S. Virgin Islands for the U.S. Geological Survey National Geospatial Program User Engagement Office and serves as a Geospatial Information Response Team Operations Officer. She is the Chair of the USGS Lidar User Group and a member of the Interagency Working Group on Ocean and Coastal Mapping, as well as the Florida Coastal Mapping Program Science and Technical Advisory Council. Xan works to help people, from USGS scientists and our Nation's residents, to a variety of agencies and entities, discover and coordinate geospatial data to empower location intelligence through outreach, collaboration, and data visualization.
Active in the American Society for Photogrammetry and Remote Sensing (ASPRS), Xan serves as Florida Region President and past GIS Division Director. She is also active in the Urban and Regional Information Systems Association (URISA), serving on the Board of Directors and as Board Liaison to the Community Resilience and Professional Education Committees. Xan is a GISCI-certified GIS Professional and earned a BS in Marine Science-Geology from Eckerd College, as well as a Postbaccalaureate Certificate in GIS and an MGIS from Penn State University.
GISCI-certified Geographic Information Systems Professional (GISP) #90578
The USGS Geospatial Information Response Team received a 2021 Esri Special Achievement in GIS award
Xan was named one of the 2021 Geospatial World 50 Rising Stars
Science and Products
Mapping Florida's Coastal Waters
The FCMaP approach divides Florida into 6 regions that are geologically and physiographically distinct in terms of coastal characteristic.
Natural Hazards, Coastal and Marine Hazards and Resources Program, St. Petersburg Coastal and Marine Science Center
The Florida Coastal Mapping Program
The Florida Coastal Mapping Program (FCMaP) is an initiative between Federal and Florida State agencies and institutions to coordinate and facilitate the collection and accessibility of Florida coastal seafloor data in order to fill priority areas and gaps.
Natural Hazards, Coastal and Marine Hazards and Resources Program, National Cooperative Geologic Mapping Program, St. Petersburg Coastal and Marine Science Center
Coastal and Marine Geology Program Lidar Coordination
Resources, publications, and contacts for lidar.
Coastal and Marine Hazards and Resources Program, St. Petersburg Coastal and Marine Science Center
TypeData ReleaseReal-time Data
Coastal Topography-Upper Florida Keys Reef Tract, Florida, 26-30 June 2016
Lidar-derived seamless (bare earth and submerged) topography Digital Elevation Model (DEM) mosaic and classified point-cloud datasets of a portion of the upper Florida Keys reef tract were produced from remotely sensed, geographically referenced elevation measurements collected June 26-30, 2016.
St. Petersburg Coastal and Marine Science Center
Coastal Topography-Chandeleur Islands, Louisiana, 23-25 June 2016
Lidar-derived seamless (bare earth and submerged) topography Digital Elevation Model (DEM) mosaic and classified point-cloud datasets of the Chandeleur Islands, Louisiana were produced from remotely sensed, geographically referenced elevation measurements collected June 23-25, 2016.
EAARL Coastal Topography-Eastern Louisiana Barrier Islands, 09 March 2008
These datasets, prepared cooperatively by the U.S. Geological Survey St. Petersburg Coastal and Marine Science Center and the National Park Service (NPS), provide lidar-derived first-surface and bare-earth topography for a portion of eastern Louisiana. Elevation measurements were acquired by the Experimental Advanced Airborne Research Lidar (EAARL) on March 9, 2008.
EAARL Coastal Topography-Northwest Florida, Post-Hurricane Katrina, 2005
These datasets, prepared by the U.S. Geological Survey St. Petersburg Coastal and Marine Science Center, provide lidar-derived first-surface and bare-earth topography for a portion of northwest Florida. Elevation measurements were acquired by the Experimental Advanced Airborne Research Lidar (EAARL) in September 2005, immediately following Hurricane Katrina landfall.
EAARL Coastal Topography-Chandeleur Islands, Post-Hurricane Katrina, 2005
These datasets, prepared by the U.S. Geological Survey St. Petersburg Coastal and Marine Science Center, provide lidar-derived first-surface and bare-earth topography for the Chandeleur Islands, Louisiana. Elevation measurements were acquired by the Experimental Advanced Airborne Research Lidar (EAARL) on September 1?4, 2005, immediately following Hurricane Katrina's landfall.
Coastal Topography - Assateague Island, Maryland and Virginia, Post-Hurricane Hermine, 10-12 September 2016
Lidar-derived seamless (bare earth and submerged) topography Digital Elevation Model (DEM) mosaic and classified point-cloud datasets were produced from remotely sensed, geographically referenced elevation measurements collected post-Hurricane Hermine on September 10-12, 2016.
EAARL Coastal Topography-Northern Assateague Island National Seashore, Maryland and Virginia, 2003: Bare Earth
These datasets, prepared by the U.S. Geological Survey St. Petersburg Coastal and Marine Science Center in collaboration with the National Park Service, provide lidar-derived bare-earth topography for Northern Assateague Island National Seashore, Maryland and Virginia. Elevation measurements were acquired by the Experimental Advanced Airborne Research Lidar (EAARL) during February 2003.
EAARL Coastal Topography-Assateague Island National Seashore, Maryland and Virginia, 2005
These datasets, prepared by the U.S. Geological Survey St. Petersburg Coastal and Marine Science Center in collaboration with the National Park Service, provide lidar-derived first-surface and bare-earth topography for Assateague Island National Seashore, Maryland and Virginia. Elevation measurements were acquired by the Experimental Advanced Airborne Research Lidar (EAARL) during September 2005.
EAARL Coastal Topography-Cape Hatteras, North Carolina, Pre- and Post-Hurricane Isabel, 2003
These XYZ datasets provide lidar-derived bare-earth topography for Cape Hatteras, North Carolina. Elevation measurements were acquired pre-Hurricane Isabel on September 16 and post-Hurricane Isabel on September 21, 2003 by the first-generation Experimental Advanced Airborne Research Lidar (EAARL), in cooperation with the National Aeronautics and Space Administration (NASA).
Coastal Topography-Long Island, New York, Post-Hurricane Irene, 30 August 2011
Lidar-derived bare-earth topography Digital Elevation Model (DEM) mosaic and classified point-cloud datasets were produced from remotely sensed, geographically referenced elevation measurements collected post-Hurricane Irene on August 30, 2011 for Long Island, New York, using a Leica ALS50-II.
Coastal Topography-Anegada, British Virgin Islands, 2014
These datasets provide lidar-derived topography for Anegada and a portion of the submerged environs. Elevation measurements were acquired on January 21, 2014 by an Optech Orion M300, and on March 19-20, 2014 by the second-generation Experimental Advanced Airborne Research Lidar (EAARL-B). The authors acknowledge Emily Klipp, Chris Pali, Virgil Rabine, Rudy Troche, and Wayne Wright, all formerly o
Publication Type (field_pub_type)
TypeArticleBookBook ChapterConference PaperOtherReportThesis
A federal-state partnership for mapping Florida's coast and seafloor
The Florida Coastal Mapping Program, a partnership of state and federal agencies, has a goal of having modern, consistent, high- resolution sea-floor data for all of Florida's coastal zone in the next decade to support a myriad of coastal zone science and management applications. One of the early steps in the implementation process is to prioritize and justify mapping needs. This is accomplished b
Florida Coastal Mapping Program—Overview and 2018 workshop report
The Florida Coastal Mapping Program is a nascent but highly relevant program that has the potential to greatly enhance the "Blue Economy" of Florida by coordinating and facilitating sea-floor mapping efforts and aligning partner and stakeholder activities for increased efficiency and cost reduction. Sustained acquisition of modern coastal mapping information for Florida may improve management of r
EAARL-B coastal topography: Chandeleur Islands, Louisiana, 2012: seamless (bare earth and submerged)
These remotely sensed, geographically referenced elevation measurements of light detection and ranging (lidar)-derived seamless (bare-earth and submerged) topography datasets were produced by the U.S. Geological Survey (USGS), St. Petersburg Coastal and Marine Science Center, St. Petersburg, Florida. This project provides datasets acquired on August 7 and 8, 2012, for a portion of the Chandeleur I
EAARL-B submerged topography: Barnegat Bay, New Jersey, pre-Hurricane Sandy, 2012
These remotely sensed, geographically referenced elevation measurements of lidar-derived submerged topography datasets were produced by the U.S. Geological Survey (USGS), St. Petersburg Coastal and Marine Science Center, St. Petersburg, Florida. This project provides highly detailed and accurate datasets for part of Barnegat Bay, New Jersey, acquired pre-Hurricane Sandy on October 18, 22, 23, an
EAARL-B coastal topography: Fire Island, New York, pre-Hurricane Sandy, 2012: seamless (bare earth and submerged)
These remotely sensed, geographically referenced elevation measurements of lidar-derived seamless (bare-earth and submerged) topography datasets were produced by the U.S. Geological Survey (USGS), St. Petersburg Coastal and Marine Science Center, St. Petersburg, Florida. This project provides highly detailed and accurate datasets for part of Fire Island, New York, acquired pre-Hurricane Sandy on
EAARL-B submerged topography: Barnegat Bay, New Jersey, post-Hurricane Sandy, 2012-2013
These remotely sensed, geographically referenced elevation measurements of lidar-derived submerged topography datasets were produced by the U.S. Geological Survey (USGS), St. Petersburg Coastal and Marine Science Center, St. Petersburg, Florida. This project provides highly detailed and accurate datasets for part of Barnegat Bay, New Jersey, acquired post-Hurricane Sandy on November 1, 5, 16, 20,
EAARL-B coastal topography: eastern New Jersey, Hurricane Sandy, 2012: first surface
These remotely sensed, geographically referenced elevation measurements of lidar-derived first-surface (FS) topography datasets were produced by the U.S. Geological Survey (USGS), St. Petersburg Coastal and Marine Science Center, St. Petersburg, Florida. This project provides highly detailed and accurate datasets for a portion of the New Jersey coastline beachface, acquired pre-Hurricane Sandy on
EAARL coastal topography and imagery–Western Louisiana, post-Hurricane Rita, 2005: First surface
These remotely sensed, geographically referenced color-infrared (CIR) imagery and elevation measurements of lidar-derived first-surface (FS) topography datasets were produced by the U.S. Geological Survey (USGS), St. Petersburg Coastal and Marine Science Center, St. Petersburg, Florida, and the National Aeronautics and Space Administration (NASA), Wallops Flight Facility, Virginia. This project p
EAARL coastal topography--North Shore, Lake Pontchartrain, Louisiana, 2010
This DVD contains lidar-derived coastal topography GIS datasets of a portion of the north shore of Lake Pontchartrain, Louisiana. These datasets were acquired on February 28, March 1, and March 5, 2010.
EAARL coastal topography--Central Wetlands, Louisiana, 2010
This DVD contains lidar-derived coastal topography GIS datasets of a portion of the Central Wetlands, Louisiana. These datasets were acquired on March 4 and 5, 2010.
EAARL coastal topography--Alligator Point, Louisiana, 2010
This project provides highly detailed and accurate datasets of a portion of Alligator Point, Louisiana, acquired on March 5 and 6, 2010. The datasets are made available for use as a management tool to research scientists and natural-resource managers. An innovative airborne lidar instrument originally developed at the National Aeronautics and Space Administration (NASA) Wallops Flight Facility, an
EAARL coastal topography-Northern Outer Banks, North Carolina, post-Nor'Ida, 2009
This DVD contains lidar-derived first-surface (FS) and bare-earth (BE) topography GIS datasets of a portion of the northern Outer Banks beachface in North Carolina. These datasets were acquired post-Nor'Ida on November 27 and 29, 2009.
Natural Hazards, Coastal and Marine Hazards and Resources Program
USGS staff from across the Coastal and Marine Hazards and Resources Program will present at the virtual Coastal GeoTools conference
Six representatives from the USGS Coastal and Marine Science Centers will present at the upcoming virtual Coastal GeoTools conference February 8–11.
CMHRP Lidar Coordinator/National Geospatial Program Associate National Map Liaison invited as Keynote speaker for the Management Association for Private Photogrammetric Surveyors 2021 Winter Meeting
Xan Fredericks, Lidar Coordinator for the Coastal and Marine Hazards and Resources Program (CMHRP) and Associate National Map Liaison to Florida...
Coastal and Marine Hazards and Resources Program Lidar Coordinator/National Geospatial Program Associate National Map Liaison elected to serve on 2020-2023 URISA Board of Directors
Xan Fredericks, Lidar Coordinator for the Coastal and Marine Hazards and Resources Program and Associate National Map Liaison to Florida, Puerto Rico...
Coastal and Marine Hazards and Resources Program (CMHRP) Lidar Coordinator/National Geospatial Program (NGP) Associate National Map Liaison hosts the first Interagency Working Group on Ocean and Coastal Mapping Meeting of 2020
Xan Fredericks, Lidar Coordinator for the CMHRP and Associate National Map Liaison to Florida, Puerto Rico, and the US Virgin Islands for the NGP...
Coastal and Marine Hazards and Resources Program (CMHRP) Lidar Coordinator/National Geospatial Program (NGP) Associate National Map Liaison attending Florida Geographic Information Office and Florida GIS Managers Quarterly Meetings
Xan Fredericks, Lidar Coordinator for the CMHRP and Associate National Map Liaison to Florida, Puerto Rico, and the US Virgin Islands for the NGP, is...
Coastal and Marine Hazards and Resources Program Lidar Coordinator/National Geospatial Program Associate National Map Liaison invited as Keynote Speaker at the 1st Annual GeoFlo Summit 2019
Xan Fredericks, Lidar Coordinator for the CMHRP and the NGP Associate National Map Liaison to Florida, Puerto Rico, and the US Virgin Islands, has...
Coastal and Marine Hazards and Resources Program (CMHRP) Lidar Coordinator/National Geospatial Program (NGP) Associate National Map Liaison presenting and moderating at the URISA GIS-Pro 2019 Conference
Coastal and Marine Hazards and Resources Program (CMHRP) Lidar Coordinator/National Geospatial Program (NGP) Associate National Map Liaison invited as Keynote Speaker at the 2019 Central Florida Geographic Information System (GIS) Workshop
Xan Fredericks, Lidar Coordinator for the CMHRP and Associate National Map Liaison to Florida, Puerto Rico, and the US Virgin Islands for the NGP, has...
CMHRP Lidar Coordinator and FCMaP Co-Chair will co-host and present at the 2019 Panhandle of Florida Seafloor Mapping Prioritization Workshop
Xan Fredericks, Lidar Coordinator for the Coastal and Marine Hazards and Resources Program and the USGS Co-Chair for the Florida Coastal Mapping...
CMHRP Lidar Coordinator/NGP Associate National Map Liaison invited as Keynote Speaker at the 2019 South Florida GIS Expo
Xan Fredericks, Lidar Coordinator for the Coastal-Marine Hazards and Resources Program and Associate National Map Liaison to Florida, Puerto Rico, and...
CMHRP Lidar Coordinator/NGP Geospatial Information Response Team member provided GIS tool demonstration to Mississippi River Cities & Towns Initiative (MRCTI) Mayors
Xan Fredericks, Lidar Coordinator for the Coastal/Marine Hazards and Resources Program and member of the National Geospatial Program's Geospatial...
CMHRP Lidar Coordinator/USGS Co-Chair of Florida Coastal Mapping Program to co-host the 2019 Northeast Florida Seafloor Mapping Prioritization Workshop


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Are you searching for a nurse that is really qualified to handle your sick child at home? Although nurses in general can take care of ailing kids, a pediatric nurse is better trained for the job. Therefore, before hiring a pediatric nurse, you need to see if the individual is really able to do what the job requires. In that regard, vetting a pediatric in-home nurse is somewhat different from vetting other kinds of nurses. Here are some tips that you need to consider.
Before anything else, you need to know if the pediatric nurse is really educated and trained in the basic rudiments of the job. That means you have to check if the person is really a BSN and is duly licensed by the professional commission in your local area. In other words, check if the nurse has a BSN degree from a reputable school and has passed the nursing licensure requirements of your country. This is just the start but it is very important to know if the nurse is really qualified and licensed before you proceed to the next vetting stage.
Of course, you can only see a person's personality after you have spent some time with her. But you can get a glimpse of the nurse's personality during the interview. Check her mannerisms, the way she answers your questions, the way she communicates and the way she presents herself. Are you sensing a positive or a negative person? You need to know because she will be taking care of your sick little child. Your kid needs a positive caring person at this time. In fact, this should be more important than the credentials that the nurse can present (although this is important too).
The nurse should be able to communicate clearly, not only with you as the parent, but more importantly with your sick kid. Hiring a pediatric nurse with good communication skills will make stressful situations more bearable. The basic approach of the nurse is to communicate with the whole family, and not just with the sick child. This healthcare service provider should realize that although the sick kid is the one who is suffering the most, it is the whole family that is affected by the sickness and not just the child.
Checking the work ethic and the reliability of a pediatric nurse is a bit tricky since you have not yet seen how she conducts herself while at work. But there should be a way in which you can assess these qualities while you are interviewing the candidate nurse. Did she come on time for the interview? Is the nurse dressed properly for the interview? Look at her past experience and perhaps you can get a glimpse of these qualities from the hospitals or clinics that the nurse has worked with.
Patience is an important requirement in child care, especially if the child is sick. And as have been mentioned previously, the PN will also be dealing with you and your family as a whole. Therefore, the nurse should also be patient with the family. The nurse should have a child care program that is family centered. The quality of patience in a person comes in developmental stages. You should see this quality as you look at the nurse's record of her past experiences.
To be effective in child care duties, the pediatric nurse should be able to think like a child. Therefore, check if the nurse is able to learn how to talk and think like a child. She should approach the child as if she is also a small kid and not as a supervising and strict adult.
A pediatric nurse should be able to relate well with small children. Without being careless and thoughtless like the average kid, the nurse should be able to go down to your child's level of thinking. She must be able to talk, think and play like a child. That's one of the best ways she can take care of your sick kid.


text:
Chichen Itza's Famous Pyramid is Actually Two Pyramids
El Castillo, or the Temple of Kukulcan, is 98 feet tall and has 365 steps. What you can't see from the outside is the original, much smaller pyramid that acted as a foundation.
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The aircraft hijacking is in the Mediterranean but the anti-hijack force is in North Carolina. That is the crux of the dilemma facing our civilian and military authorities charged with overseeing this nation's strengthened anti- terrorist policies and forces. It is a long haul for the crack Delta Force commandos in North Carolina to the scene of a piracy or other terrorist action - made even more so by the time factor imposed by the deadliness of the deed.
For that reason, the Reagan administration has proposed moving at least portions of the U.S. anti-terrorist organizations closer to the site of a potential hijack. In recent months, this has been primarily in or near the volatile Middle East. To position a permanent, yet highly mobile, force stationed in, for example, West Germany, Italy or even on a Sixth Fleet aircraft carrier, is the administration's wish. That is a move so logical in concept that one wonders why it had not been examined earlier. Surely, the presence of a Delta Force strike team only several hundred miles, rather than several thousand miles, from a hijacked aircraft will serve as an assurance of swift, surgical action by thishighly trained group. The worth of its technical expertise and deftness was proven graphically by its advisory role to Venezuelan troops who stormed a hijacked jet in August 1984, killing two terrorists - with no other loss of life.
Perhaps, however, there is one more logical step that can be recommended in the international war against terrorism. Perhaps the formation of a multi- national anti-terror force should be considered. Imagine the widened scope and increased availability of materiel and intelligence that a combined group of, say, Delta Force commandos, Israeli experts, British Special Air Services troops and their counterparts from other countries would command. In addition, the mixture of nationalities might overcome the reluctance of nations such as Malta and others to allow foreign - specifically American - military personnel on their soil, as was the case in the recent tragedy on that Mediterranean island nation.
Hijacking and killing and terror as political acts are a world menace. Would it not be wise to consider working with the majority of the rest of the world community in an effort to create a unified force with which to respond, with speed and strength, to the heinous actions of the terrorists?


text:
\section{Introduction}

Outflows in the form of jets and winds are observed from many disc accreting
objects ranging from young stars to systems with white
dwarfs, neutron stars, and black holes.
   A large body of observations exists for outflows
from young stars at different stages of their
evolution, ranging from protostars, where powerful
collimated outflows -  jets -  are observed, to classical T Tauri stars (CTTSs) where the outflows are weaker and often  less collimated (see review by Ray et al. 2007).
Correlation between the disc's radiated power and the jet power has been found in many CTTSs (Cabrit et al. 1990;
 Hartigan, Edwards \& Gandhour 1995).
A significant number of CTTSs show signs
of outflows in spectral lines, in particular in
He I where two distinct components of outflows
had been found (Edwards et al. 2003, 2006; Kwan, Edwards, \& Fischer 2007).
 Outflows are also observed from accreting compact stars such as accreting white dwarfs in symbiotic binaries (Sokoloski \& Kenyon 2003),
or from the vicinity of neutron stars, such as from  Circinus X-1 (Heinz et al. 2007).

Different theoretical models have been proposed
to explain the outflows from protostars and CTTSs
(see review by Ferreira, Dougados, \& Cabrit 2006).
The models include those where the outflow
originates from a radially distributed disc
wind (Blandford \& Payne 1982; K\"onigl \& Pudritz 2000;
Casse \& Keppens 2004; Ferreira et al. 2006) or
from the innermost region of the accretion disc (Lovelace, Berk \& Contopoulos 1991).    The latter model is related to the
 X-wind  model (Shu et al. 1994; 2007; Najita \& Shu 1994; Cai et al. 2008) where
the outflow originates from the vicinity of the disc-magnetosphere boundary.
Progress in understanding the theoretical models
has come from MHD simulations of accretion discs around rotating
magnetized stars as discussed below.    Laboratory experiments are
also providing insights into jet formation processes (Hsu \& Bellan 2002;
Lebedev et al. 2005) but these are not discussed here.

Outflows or jets from the disc-magnetosphere boundary were found in early axisymmetric MHD simulations by
Hayashi, Shibata \& Matsumoto (1996) and  Miller \& Stone (1997).
A one-time episode
of outflows from the inner disc and inflation of the
innermost field lines connecting the star and the disc were observed
for a few dynamical time-scales.
        Somewhat longer simulation runs were performed
 by Goodson et al. (1997, 1999), Hirose et al. (1997),
Matt et al. (2002) and K\"uker, Henning \& R\"udiger (2003)
where several episodes of field inflation and outflows were observed.
These simulations hinted at a possible long-term nature for the outflows.
 However,  the simulations were not sufficiently long to establish
the behavior of the outflows.
     MHD simulations showing long-lasting (thousand of
orbits of the inner disc)  outflows from the disc-magnetosphere have been obtained by our group
 (Romanova et al. 2009;  Lii et al. 2012).
   We obtained these outflows/jets
in two main cases: (1) where the star rotates slowly but the field lines are bunched up into an X-type configuration,  and (2) where
the star rotates rapidly, in the ``propeller regime''
(Illarionov \& Sunyaev 1975;
Alpar \& Shaham 1985; Lovelace, Romanova \& Bisnovatyi-Kogan 1999) .
    Figure 1 shows the equatorial angular rotation rate $\Omega(r,z=0)$
of the plasma in the two cases.   Here,  $r_*$ is the radius
of the star;  $r_{\rm m}$ is the magnetospheric radius where the
kinetic energy density of the disc matter is about equal to the   energy
density of the magnetic field; and
$r_{\rm cr}= (GM/\Omega_*^2)^{1/3}$
is the co-rotation radius where the angular rotation rate of the
star $\Omega_*$ equals that of the Keplerian disc $\Omega_K=
(GM/r^3)^{1/2}$.    For a slowly rotating star $r_{\rm m} < r_{\rm cr}$
whereas for a rapidly rotating star in the propeller regime
$r_{\rm m} >r_{\rm cr}$.

\begin{figure}
\begin{center}
  \includegraphics[width=5in]{Fig1.eps}
  \caption{Schematic profiles of the midplane angular velocity
  of the plasma for the case of a slowly rotating star (left-hand panel)
  and a rapidly rotating star (right-hand panel) which is in the
  propeller regime.  Here, $\Omega_*$ is the angular
  rotation rate of the star, $\Omega_K$ is the Keplerian rotation
  rate of the disc,  $r_*$ is the star's radius, $r_{\rm m}$ is the
  radius of the magnetosphere, and $r_{\rm cr}$ is the co-rotation
  radius.}
  \end{center}
\end{figure}

       Figure 2 shows examples of the outflows in the
two cases.
In both cases, two-component outflows are observed:
One component originates at the inner edge
of the disc  near $r_{\rm m}$ and has a narrow-shell conical shape close to the disc and therefore is termed a ``conical wind".   It is matter dominated
but can become collimated at large distances due to its toroidal magnetic
field.
The other component is a magnetically dominated high-velocity
``axial jet'' which flows along the open stellar magnetic field lines.
             The axial jet may be very strong in the propeller regime.
  A detailed discussion of the simulations and analysis can
be found in Romanova et al. (2009) and Lii et al. (2012).

     Sec. 2 describes the simulations.   Sec. 3 discusses the conical winds and axial jets, the driving and collimation forces, and the variability of
the winds and jets.  Sec. 4 discusses simulation
results on one-sided and lop-sided jets.  Sec. 5 gives the conclusions.

\begin{figure}
\begin{center}
  \includegraphics[width=5.in]{Fig2.eps}
  \caption{Two-component outflows observed in slowly (left) and rapidly (right) rotating magnetized stars adapted from Romanova et al. (2009).
The background shows
the poloidal matter flux $F_m=\rho v_p$, the arrows are the  poloidal
velocity vectors, and the lines are sample magnetic field lines.
The labels point to the main outflow components.}
\end{center}
\end{figure}

\section{MHD Simulations}

We simulate the outflows resulting from disc-magnetosphere interaction
using the equations of axisymmetric MHD.

Outside of the disc the flow is described by the
equations of ideal MHD.
     Inside the disc the flow is described by
the equations of viscous, resistive MHD.
In an inertial reference frame the equations are:
\begin{equation}\label{eq1}
\displaystyle{ \frac{\partial \rho}{\partial t} + {\bf \nabla}\cdot
\left( \rho
{\bf v} \right)} = 0~,
\end{equation}
\begin{equation}\label{eq2}
{\frac{\partial (\rho {\bf v})}{\partial t} + {\bf
\nabla}\cdot
{\cal T} } = \rho ~{\bf g}~,
\end{equation}
\begin{equation}\label{eq3}
{\frac{\partial {\bf B}}{\partial t} - {\bf
\nabla}\times ({\bf v} \times {\bf B}) + {\bf \nabla} \times\left(
\eta_t {\bf \nabla}\times {\bf B} \right)} = 0~,
\end{equation}
\begin{equation}\label{eq4}
{\frac{\partial (\rho S)}{\partial t} + {\bf
\nabla}\cdot ( \rho S {\bf v} )} =  Q~.\
\end{equation}
 Here, $\rho$ is the density,  $S$ is the specific entropy, $\bf
v$ is the flow velocity, $\bf B$ is the magnetic field, $\eta_t$
is the  magnetic diffusivity,  $\cal{T}$ is the
momentum flux-density tensor, $Q$ is
the rate of change of entropy per unit volume,  and ${\bf g} = - (GM /r^{2})\hat{{\bf r}}$
is the gravitational acceleration due to the star, which has mass $M$.
The total mass of the disc is assumed to
be negligible compared to $M$.
    Here, ${\cal T}$ is the sum of the ideal plasma terms {\it and}
the $\alpha-$viscosity terms discussed in the next paragraph.
     The  plasma is considered to be an
ideal gas with adiabatic index $\gamma =5/3$, and $S=\ln(p/
\rho^{\gamma})$. We use spherical coordinates $(r, \theta, \phi)$ with  $\theta$ measured from the symmetry axis.
 The  equations in spherical coordinates are given in
Ustyugova et al. (2006).

     Both the viscosity
and the magnetic diffusivity of the disc plasma are considered
to be due to turbulent fluctuations of the velocity and the magnetic field.
Both effects are non-zero only inside the disc as determined by
a density threshold.
       The  microscopic transport coefficients are  replaced by
 turbulent coefficients.
       The values of these coefficients are assumed to be given by
the  $\alpha$-model of Shakura and Sunyaev (1973), where the
coefficient of the turbulent kinematic viscosity is $\nu_t =
\alpha_\nu c_s^{2}/\Omega_K$, where $c_s$ is the isothermal sound
speed and $\Omega_K(r)$ is the Keplerian angular velocity.
We take into account the viscous stress terms ${\cal T}_{r\phi}^{\rm vis}$
and ${\cal T}_{\theta \phi}^{\rm vis}$ (Lii et al. 2012).
        Similarly, the coefficient of the turbulent magnetic
diffusivity $\eta_t=\alpha_\eta c_s^{2}/\Omega_K$. Here,
      $\alpha_\nu$ and $\alpha_\eta$ are dimensionless coefficients which
are treated as parameters of the model.

The MHD equations are solved in
dimensionless form so that the results can be readily applied
to different accreting stars.

\begin{table*}
\centering
\caption{Reference values for different types of stars. We choose the mass $M$, radius $R_*$,
equatorial magnetic field $B_*$ and  the period $P_*$ of the star and derive the other reference values.
   The reference
mass $M_0$ is taken to be the mass $M$ of the star.
  The reference radius is taken to be twice the radius
of the star, $R_0=2 R_*$.
    The surface
magnetic field $B_*$ is
different for different types of stars.
  The reference velocity is $v_0=(GM/R_0)^{1/2}$.
The reference time-scale $t_0=R_0/v_0$, and the reference angular velocity $\Omega_0=1/t_0$.
    We measure time
in units of $P_0=2\pi t_0$ (which is the Keplerian rotation period at $r=R_0$).
In the plots we  use the dimensionless time $T=t/P_0$.
    The reference magnetic field is $B_0=B_*(R_*/R_0)^{3}/{\tilde\mu}$,
where $\tilde\mu$ is the dimensionless magnetic moment which has
a numerical value of $10$ in the simulations discussed here.
    The reference density is taken to
be  $\rho_0 = B_0^{2}/v_0^{2}$.
The reference pressure is $p_0=B_0^{2}$.
The reference temperature is
$T_0=p_0/{\cal R} \rho_0 = v_0^{2}/{\cal R}$, where ${\cal R}$ is the gas constant.
   The reference accretion rate is $\dot M_0
= \rho_0 v_0 R_0^{2}$.
   The reference energy flux is $\dot
E_0=\dot M_0 v_0^{2}$.
The reference angular momentum flux is $\dot{L}_0=\dot M_0 v_0
R_0$.   The poloidal  magnetic field
of the star (in the absence of external plasma) is an aligned dipole field.
}
\begin{tabular}{l@{\extracolsep{0.2em}}l@{}lllll}

\hline
&                                              & Protostars      & CTTSs        & Brown dwarfs   & White dwarfs        & Neutron stars    \\
\hline

\multicolumn{2}{l}{$M(M_\odot)$}                  & 0.8            & 0.8            & 0.056             & 1                   & 1.4       \\
\multicolumn{2}{l}{$R_*$}                         & $2R_\odot$     & $2R_\odot$     & $0.1R_\odot$       & 5000 km             & 10 km     \\
\multicolumn{2}{l}{$R_0$ (cm)}                    & $2.8\cdot10^{11}$    & $2.8\cdot10^{11}$    & $1.4\cdot10^{10}$      & $10^9$            & $2\cdot10^6$    \\
\multicolumn{2}{l}{$v_0$ (cm s$^{-1}$)}           & $1.95\cdot10^7$      & $1.95\cdot10^7$      & $1.6\cdot10^7$          & $3.6\cdot10^8$   & $9.7\cdot10^{9}$ \\
\multicolumn{2}{l}{$P_*$}                         & $1.04$ days    & $5.6$ days     & $0.13$ days        & $89$ s              & $6.7$ ms     \\
\multicolumn{2}{l}{$P_0$}                         & $1.04$ days    & $1.04$ days    & $0.05$ days       & $17.2$ s            & $1.3$ ms   \\
\multicolumn{2}{l}{$B_*$ (G)}                      & $3.0\cdot10^3$      & $10^{3}$      & $2\cdot10^{3}$            & $10^{6}$            & $10^{9}$    \\
\multicolumn{2}{l}{$B_0$ (G)}                     & 37.5           & 12.5          & 25.0                & $1.2\cdot10^4$            & $1.2\cdot10^{7}$  \\
\multicolumn{2}{l}{$\rho_0$ (g cm$^{-3}$)}         & $3.7\cdot10^{-12}$  & $4.1\cdot10^{-13}$  & $1.4\cdot10^{-12}$        & $1.2\cdot10^{-9}$         & $1.7\cdot10^{-6}$  \\
\multicolumn{2}{l}{$n_0$ (cm$^{-3}$)}            & $2.2\cdot10^{12}$   & $2.4\cdot10^{11}$   & $8.5\cdot10^{11}$         & $7\cdot10^{14}$         & $10^{18}$          \\
\multicolumn{2}{l}{$\dot M_0$($M_\odot$yr$^{-1}$)}  & $1.8\cdot10^{-7}$  & $2\cdot10^{-8}$   & $1.8\cdot10^{-10}$      & $1.3\cdot10^{-8}$         & $2\cdot10^{-9}$  \\
\multicolumn{2}{l}{$\dot E_0$ (erg s$^{-1}$)}       & $2.1\cdot10^{33}$  & $2.4\cdot10^{32}$   & $2.5\cdot10^{30}$      & $5.7\cdot10^{34}$         & $6\cdot10^{36}$  \\
\multicolumn{2}{l}{$\dot L_0$ (erg s$^{-1}$)}       & $3.1\cdot10^{37}$  & $3.4\cdot10^{36}$   & $1.7\cdot10^{33}$      & $1.6\cdot10^{35}$         & $1.2\cdot10^{33}$  \\
\multicolumn{2}{l}{$T_d$ (K)}                       & $2290$       & $4590$        & $5270$            & $1.6\cdot10^{6}$          & $1.1\cdot10^{9}$  \\
\multicolumn{2}{l}{$T_c$ (K)}                       & $2.3\cdot10^{6}$   & $4.6\cdot 10^{6}$    & $5.3\cdot10^{6}$        & $8\cdot10^{8}$          & $5.6\cdot10^{11}$  \\
\hline
\end{tabular}
\end{table*}

The system of MHD equations (1-4) have been
 integrated numerically in spherical $(r,\theta,\phi)$ coordinates
  using a Godunov-type numerical scheme.
The calculations were done
in the region $R_{\rm in} \leq r \leq R_{\rm out}$, $0\leq \theta
\leq \pi/2$. The grid is uniform in the $\theta$-direction with $N_\theta$ cells.
    The $N_r$ cells in the radial direction  have $ dr_{j + 1} = (1 + 0.0523)dr_j$ ($j=1..N_r$) so
 that the poloidal-plane cells are curvilinear rectangles with approximately
equal sides.    This choice results in high spatial resolution near the star
where the disc-magnetosphere interaction takes place while
also permitting a large simulation region.
    We have used a range of resolutions going from
 $N_r\times N_\theta = 51\times 31$  to $121\times 51$.

\begin{figure*}
\centering
\includegraphics[width=5in]{Fig3.eps}
\caption{Matter flux $\rho v_p$ (background), sample field lines, and poloidal velocity vectors in a propeller-driven outflow at time $t=1400$ (rotations at $r=1$) adapted from Romanova et al. (2009).
Sample numerical values are given for the poloidal $v_p$ and  total $v_t$ velocity, and for the density $\rho$ for different parts of the simulation region.
One can see from the Table 1 that for CTTSs $v_p=1$ corresponds to $v_p=195$ km/s in dimensional units.
   Unit density corresponds to $\rho_0=4.1\times 10^{-13}$ g cm$^{-3}$. Dimensionless data shown on the plot can be converted to dimensional units for other types of stars  using the reference values from the Table 1.}
\end{figure*}

\section{Conical Winds and  Axial Jets}

      A large number of simulations were done in order
to understand  the origin and nature of conical winds.
  All of the key parameters were varied in order   to ensure that
 there is no special  dependence on any parameter.
  We observed that the formation of conical winds
is a common phenomenon for a wide range of parameters.
They are most persistent and strong in cases where
the  viscosity and diffusivity coefficients are not very
small, $\alpha_\nu\gtrsim 0.03$, $\alpha_\eta \gtrsim 0.03$.
Another important condition is  that $\alpha_\nu \gtrsim\alpha_\eta$;
that is, the magnetic Prandtl number
of the turbulence, ${\cal P}_m=\alpha_\nu/\alpha_\eta \gtrsim 1$.
This condition favors the bunching of the stellar magnetic
field by the accretion flow.

       Figure 3 shows a  snapshot from our simulations at time $t=1400$ for  the propeller regime.
The figure shows the dimensionless density and velocity at sample points.
One can see that the velocities in the conical wind component are similar to those in conical winds around slowly rotating stars.
  Matter launched from the disc initially has
an  approximately Keplerian  azimuthal velocity, $v_K=\sqrt{GM_*/r}$.
   It is gradually accelerated to poloidal velocities $v_p\sim (0.3-0.5) v_K$
and the azimuthal velocity decreases.
The flow has a high density and carries most of the disc mass into the outflows.
The situation is the opposite in the axial jet component where the density is $10^2-10^3$ times lower, while the poloidal and total velocities are
significantly  higher.
   Thus we find a  {\it two-component outflow}:  a matter
 dominated conical wind and a magnetically dominated axial jet.

\begin{figure*}
\centering
\includegraphics[width=5in]{Fig4.eps}
\caption{The conical wind/jet from a slowly rotating star
at time $t= 860$ adapted from Lii et al. (2012).
The background shows the poloidal matter flux density $\rho{\bf v}_p$ and the lines show
the poloidal projections of the magnetic magnetic field.
The red vectors show the poloidal matter velocity ${\bf v}_p$.
Dimensional values can be obtained from Table 1.
For example for a CTTS, $t_0 = 0.366$ days, $R_0= 2\ensuremath{{\rm R}_{\odot}}$,  $ t=860$ corresponds
to $315$ days,  and the simulation region is $0.39$ AU in radius.
The horizontal axis shows the distance  from the star in units of the reference radii $R_0$.  For this case $\alpha_\nu=0.3$ and $\alpha_\eta=0.1$. }
\end{figure*}

   We observe conical winds in both slowly and rapidly rotating stars.
In both cases, matter in the conical winds passes through the Alfv\'en surface
(and shortly thereafter through the fast magnetosonic point),
beyond which the flow is matter-dominated in the sense that the energy flow is carried mainly by the matter.
    The situation is different for the axial jet component where the flow
is sub-Alfv\'enic within the simulation region.
   For this component the energy flow is carried by the
 Poynting flux and the angular moment flow is carried by the
 magnetic field.

 \noindent{\bf Collimation and Driving of the Outflows:}
 Figure 4 shows the long-distance development of a conical wind from a slowly rotating star.   At large distances
the conical wind becomes collimated.

   To understand the collimation we analyzed
total force (per unit mass)
perpendicular to a poloidal magnetic field line (Lii et al. 2012).
For distances beyond the Alfv\'en surface of the flow this
force is approxiamtely
\begin{equation}
f_{\rm tot, \perp}  = - v_{\rm p}^2 \frac{\partial \Theta}{\partial s}
 - \frac{1}{8\pi \rho}\frac{\partial{\bf B}_p^2}{\partial n}
 -\frac{1}{8\pi\rho (r\sin\theta)^2}\frac{\partial(r\sin\theta B_\phi)^2}{\partial n} + \frac{v_\phi^2}{r}\frac{\cos\Theta}{\sin\theta}.
\end{equation}
(Ustyugova et al. 1999).  Here, $\Theta$ is the angle between the poloidal magnetic field and the symmetry axis, $s$ is the arc length
along the poloidal field line, $n$ is a coordinate normal to
the poloidal field,  and the $p-$subscripts indicate
the poloidal component of a vector.
Once the jet begins to collimate, the curvature term $-v_{\rm p}^2\partial \Theta/\partial s$ also becomes negligible.
      The magnetic force may act to either collimate or decollimate the jet, depending on the relative magnitudes of the toroidal $(r\sin\theta B_\phi)^2$ gradient (which collimates the outflow) and poloidal ${\mathbf B}_p^2$ gradient (which ``decollimates'').
        In our simulations, the collimation of the matter implies that the magnetic hoop stress is larger than the poloidal field gradient. Thus the main perpendicular forces acting in the jet are the collimating effect of the toroidal magnetic field and the decollimating effect of the centrifugal force
and the gradient of ${\bf B}_p^2$.  The collimated effect of $B_\phi$ dominates.   Note that in MKS units  $2\pi r\sin\theta B_\phi/\mu_0$ is the poloidal current flowing through a surface of radius $r$ from colatitude zero to $\theta$.  For the jets from young stars this current is of the order of
$2 \times 10^{13}$ A.

\begin{figure*}[b]
\centering
\includegraphics[width=5.in]{Fig5.eps}
\caption{Forces along a field line in the jet adapted from Lii
et al. (2012).
{\bf Panel (a)} shows the poloidal matter flux density \ensuremath{\rho \left| {\mathbf{v}_p} \right|}\ as a background overplotted with poloidal magnetic field lines. The vectors show the {\it total} force ${\mathbf f}_{\rm tot}$ along a representative field line originating from the disk at $r = 1.24$.
{\bf Panel (b)} plots the angular velocity $\Omega$ as the background. The vectors show the sum of the {\it gravitational + centrifugal} forces ${\mathbf f}_{\rm G+C}$ along the representative field line.
{\bf Panel (c)} shows the poloidal current $I_p$ as the background. The vectors show the total {\it magnetic} force ${\bf f}_{\rm M}$ along the representative field line. }
\end{figure*}

        The driving force for the outflow
is simply the force parallel to the poloidal magnetic field of the flow $f_{{\rm tot},\parallel}$.
  This is obtained by taking the dot product of the Euler equation with the $\hat{\mathbf b}$ unit vector which is parallel to the poloidal magnetic field line ${\mathbf B}_p$.    The derivation by Ustyugova et al. (1999) gives
\begin{equation}
f_{\rm tot, \parallel}
 =  - \frac{1}{\rho}\frac{\partial P}{\partial s} - \frac{\partial \Phi}{\partial s} + \frac{v_\phi^2}{r\sin\theta} \sin\Theta + \frac{1}{4 \pi \rho} \hat{\mathbf b} \cdot [(\nabla \times \bvec) \times \bvec].
\end{equation}
Here,  the terms on the right-hand side correspond to the
 pressure, gravitational, centrifugal and magnetic forces, respectively
 denoted ${\bf f}_{\rm P, G, C, M}$.
      The pressure gradient force, ${\bf f}_{\rm P}$, dominates within the disk. The matter in the disk is approximately in Keplerian rotation such that the sum of the gravitational and centrifugal forces roughly cancel (${\bf f}_{\rm G+C} \approx 0$). Near the slowly rotating star, however, the matter is strongly coupled to the stellar magnetic field and the disk orbits at sub-Keplerian speeds, giving ${\bf f}_{\rm G+C} \mathrel{\hbox{\rlap{\hbox{\lower4pt\hbox{$\sim$}}}\hbox{$<$}}} 0$.
    The  magnetic
 driving force (the last term of Eq. 6) can be expanded as
\begin{equation}
f_{\rm M, \parallel}
 = -\frac{1}{8 \pi \rho (r\sin\theta)^2}{\partial \over \partial s}
 (r\sin\theta B_\phi)^2~,
\end{equation}
(Lovelace et al. 1991).

    Figure 5 shows the variation of the total force ${\bf f}_{\rm tot}$,
 the gravitational plus centrifugal force, and the magnetic force
 along a representative field line.
 This analysis establishes that the predominant driving force for the outflow is the magnetic force (Eq. 7) and not the centrifugal force.
   This in agreement with the analysis of Lovelace et al. (1991).

  {\bf Variability:}   For both rapidly and slowly
rotating stars     the magnetic field lines
connecting the disc and the star have the tendency to
inflate and open (Lovelace,  Romanova \& Bisnovatyi-Kogan 1995).
Quasi-periodic reconstruction of the magnetosphere due to
inflation and reconnection has been discussed theoretically (Aly
\& Kuijpers 1990) and has been
observed in a number of axisymmetrtic simulations (Hirose et al.
1997; Goodson et al. 1997, 1999; Matt et al. 2002; Romanova et al.
2002).  Goodson \& Winglee (1999) discuss the physics of inflation cycles.
They have shown that each cycle of inflation
consists of a period of matter accumulation near
the magnetosphere, diffusion of this matter through the magnetospheric field,
inflation of the corresponding field lines,
accretion of some matter onto the star, and outflow of some matter as winds,
 with subsequent expansion of the magnetosphere. There simulations show $5-6$
 cycles of inflation and reconnection.
 Our simulations often show $30-50$ cycles of inflation and reconnection.
    Figure 6 shows the time evolution of the accretion rates
for a of a slowly rotating star (Romanova et al. 2009).

\begin{figure*}[h]
\centering
\includegraphics[width=3.in]{Fig6.eps}
\caption{Matter flux onto the star $\dot M_s$, into the
conical wind $\dot M_w$, and through the disk $\dot M_d$. }
\end{figure*}

\begin{figure*}[h]
\centering
\includegraphics[width=4.in]{Fig7.eps}
\caption{The initial poloidal magnetic field lines
and constant magnetic pressure lines for
the case of an aligned dipole and quadrupole field adapted from
Lovelace et al. (2010).
The funnel flow (ff) and the wind in this figure are suggested.
The dashed lines are constant values of ${\bf B}^2$.}
\end{figure*}

Kurosawa and Romanova (2012) have calculated spectra from modeled conical winds using the radiative transfer code TORUS
and have shown that conical winds may explain different features in the hydrogen spectral lines,  in the He I line and
also a relatively narrow, low-velocity blue-shifted absorption
components in the He I $\lambda 10830$ which is often seen in observations (Kurosawa et al. 2011).

\section{One-Sided and Lop-Sided Jets}

There is clear evidence,  mainly from
Hubble Space Telescope (HST) observations,  of the asymmetry
between the approaching and receding jets
from a number of young stars.
The objects include the jets in HH 30 (Bacciotti et al. 1999),
RW Aur (Woitas et al. 2002), TH 28 (Coffey et al. 2004),
and LkH$\alpha$ 233  (Perrin \& Graham 2007).
  Specifically, the radial speed of the approaching
jet may differ by a factor of two from that of
the receding jet.
    For example, for RW Aur the radial redshifted
speed is $\sim 100$ km/s whereas the blueshifted
radial speed is $\sim175$ km/s.
   The mass and momentum fluxes are also
significantly different
for the approaching and receding jets in a number of cases.
  Of course, it is possible that the observed asymmetry
of the jets could be due to say differences in the gas densities
on the two sides of the source.   Here, we discuss
the case of intrinsic asymmetry where the asymmetry of outflows is
connected with asymmetry of the star's magnetic field.
      Substantial  observational evidence points to the fact that
young stars often have {\it complex} magnetic  fields consisting
of    dipole,  quadrupole, and higher order  poles
misaligned with respect to each other and the rotation
axis (Jardine et al. 2002; Donati et al.  2008).
Analysis of the plasma flow around stars with realistic fields
have shown that a fraction
of the star's magnetic field lines are open
and may carry outflows (e.g., Gregory et al. 2006).

        It is evident that the  complex magnetic field
of a star will destroy the commonly assumed symmetry of the magnetic field and the plasma about the equatorial plane.
   Figure 7 shows an illustrative complex magnetic field consisting of
the combination of a dipole and a quadrupole field both of which are axisymmetric.
The figure includes the suggested locations of the funnel
flow to the star (Romanova et  al. 2002) and the conical wind outflows.
   The MHD simulations fully support the qualitative picture
suggested in Figure 7 (Lovelace et al. 2010).  The time-scale during
which the jet comes from the upper hemisphere is set
by the evolution time-scale for the stellar magnetic field.
This is determined by the dynamo processes responsible for
the generation of the field.

      Remarkably, once the assumption of symmetry about the
equatorial plane is dropped, we find that the conical winds
alternately come from one hemisphere and then the other
{\it even} when the stellar magnetic field is a centered
axisymmetric dipole  (Lovelace et al. 2010).
An illustrative case of this spontaneous symmetry breaking is shown
in Figure 8.  The time-scale for the `flipping' is the accretion time-scale
of the inner part of the disc which is expected to be much less
than the evolution time of the star's magnetic field.

\begin{figure*}[t]
\centering
\includegraphics[width=5.in]{Fig8.eps}
\caption{"Flip-flop"of outflows in the case
where the stellar magnetic field is a
centered axisymmetric dipole adapted from Lovelace
et al. (2010).
The color background shows the matter flux
distribution, and the lines are the poloidal magnetic field lines.}
\end{figure*}

\section{Conclusions}

      Detailed magnetohydrodynamic simulations have
established that long-lasting outflows of  cold disc matter into a hot low-density corona from the disc-magnetosphere boundary in cases of slowly and rapidly rotating stars.  The main results are the following:

  For slowly rotating stars
a new type of outflow ---  a conical wind --- has been discovered.
  Matter flows out forming a {\it conical wind} which has the shape of a thin conical shell with a half-opening angle $\theta \sim 30^\circ$.
The outflows appear in cases where the magnetic flux of the star is bunched up by the inward accretion flow of the disc.
We find that this occurs when the turbulent magnetic Prandtl number
(the ratio of viscosity to diffusivity)  ${\cal P}_m > 1$, and when the viscosity is sufficiently high, $\alpha_\nu\gtrsim 0.03$.

Winds from the disc-magnetosphere boundary
have been proposed earlier by Shu and collaborators and referred to as
X-winds (Shu et al. 1994).
In this model,  the wind originates from a small region near the corotation radius $r_{\rm cr}$,
while the disc truncation radius $r_t$ (or, the magnetospheric radius $r_{\rm m}$) is only slightly smaller than
$r_{\rm cr}$ ($r_{\rm m}\approx 0.7 r_{\rm cr}$, Shu et al. 1994).
   It is suggested that excess angular
momentum flows  from the star to the disc and from there into the X-winds.
  The model aims to explain the slow rotation of the star and the formation of jets.
In the simulations discussed here we have  obtained outflows from both
slowly and rapidly rotating stars.
Both have conical wind components which are reminiscent of  X-winds.
     In some respects  the conical winds are similar to
X-winds:  They both require {\it bunching} of the poloidal field lines and show outflows from the inner disc; and they both have high rotation and show gradual poloidal acceleration (e.g., Najita \& Shu 1994).

       The main differences are the following:
{(1)} The conical/propeller outflows have {\it two components}: a slow high-density  conical wind (which can be considered as an analogue of the X-wind), and a fast low-density jet.
No jet component is discussed in the X-wind model.
{(2)} Conical winds form around stars with {\it any rotation rate} including very slowly rotating stars. They do not require fine tuning of the corotation and truncation radii.
For example, bunching  of field lines is often expected during periods of enhanced or unstable accretion when the disc comes closer to the surface of
the star and  $r_{\rm m}<<r_{\rm cr}$. Under this condition conical winds will form. In contrast, X-winds require $r_{\rm m}\approx r_{\rm cr}$.~ { (3)}
The base of the conical wind component in both slowly and rapidly rotating stars is associated with the region where the field lines are bunched up, and not with the corotation radius.
{(4)} X-winds are driven by the {\it centrifugal force}, and as a result matter flows over a wide range of directions below the ``dead zone"   (Shu et al. 1994; Ostriker \& Shu 1995).
In conical winds the matter is driven by the {\it magnetic force} (Lovelace et al. 1991) which acts such that
the matter flows into a {\it thin shell} with a cone half-angle $\theta\sim 30^\circ$. The same force tends to  collimate the flow.

   For rapidly rotating stars in the propeller regime where
$r_{\rm m} > r_{\rm cr}$ and where the condition for bunching, ${\cal P}_m>1$, is satisfied
we find two distinct outflow components (1) a relatively low-velocity conical wind and (2) a high-velocity axial jet.
 A significant part of the disc matter and  angular momentum flows into the conical winds.
   At the same time a significant part of the rotational energy of the star flows
into the magnetically-dominated axial jet.
   This regime is particularly relevant to protostars, where the star rotates rapidly and has a high accretion rate.
   The star spins down rapidly due to the angular momentum flow into the axial jet along the field lines connecting the star and the corona. For typical parameters a protostar spins down in $3\times10^5$ years. The axial jet is powered by the spin-down of the star rather than by disc accretion.
    The matter fluxes into both components (wind and jet) strongly oscillate due to events of inflation and reconnection. Most powerful outbursts occur every $1-2$ months. The interval between outbursts is expected to be longer for smaller diffusivities in the disc.
Outbursts are accompanied by higher outflow velocities and stronger self-collimation of both components. Such outbursts may
explain the ejection of knots in some CTTSs every few months.

      When the artificial requirement of symmetry about the
equatorial plane is dropped,  MHD simulations reveal
that  the conical winds may
alternately come from one side of the disc and then the other
even for the case where the stellar magnetic field is a
centered axisymmetric dipole (Lovelace et al. 2010).

   In recent work we have studied the disc accretion
to rotating magnetized stars in the propeller regime
using a new code with very high resolution in the region
of the disc (Lii et al. 2013).
In this code  {\it no} turbulent viscosity or diffusivity is incorporated,
but instead strong turbulence occurs due to the magneto-rotational
instability.  This turbulence drives the accretion and it leads
to  episodic outflows.

The authors thank G.~V. Ustyugova and A.~V. Koldoba for the development of the codes used in the
reported simulations.   This research was supported in part by NSF grants AST-1008636 and AST-1211318 and by a NASA ATP grant NNX10AF63G; we thank NASA for use of the NASA High Performance Computing Facilities.

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\end{harvard}

\end{document}

redpajama_set_name: RedPajamaArXiv


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text:
YouTube's Parent Google is a Corporate Member of the Council on Foreign Relations
May 5, 2009 Comments
As Paul Joseph Watson and Kurt Nimmo note today, Google is in bed with the CIA. In 2006, Robert David Steele, a 20-year Marine Corps infantry and intelligence officer and a former clandestine services case officer with the CIA, told Alex Jones as much. Steele went so far as to name Dr. Rick Steinheiser as the CIA's liaison at Google.
But it is not simply the CIA. Google is high up on the elitist NWO pyramid, a fact pointed out by an Infowar's reader and missed by the editors. As it turns out, Google is a corporate member of the Council on Foreign Relations. In late 2006, Google bought YouTube for US$1.65 billion in stock, so it is fair to say YouTube is also pushing the CFR's one-world government agenda.
[efoods]It also explains why YouTube is going after Alex Jones and why The Alex Jones Channel was scrubbed from the popular website.
"The CFR is the American Branch of a society which originated in England, and which believes that national boundaries should be obliterated, and a one-world rule established," the late Carroll Quigley wrote in his book, "Tragedy & Hope."
"The ultimate aim of the CFR is to create a one-world socialist system, and to make the U.S. an official part of it," explained Dan Smoot, a former member of the FBI Headquarters staff in Washington, D.C.
"The CFR is the establishment," writes Congressmen John R. Rarick. "Not only does it have influence and power in key decision-making positions at the highest levels of government to apply pressure from above, but it also finances and uses individuals and groups to bring pressure from below, to justify the high level decisions for converting the U.S. from a sovereign Constitution Republic into a servile member of a one-world dictatorship."
CFR "members have run, or are running, NBC and CBS, 'The New York Times', 'The Washington Post', 'The Des Moines Register', and many other important newspapers. The leaders of 'Time', 'Newsweek', 'Fortune', 'Business Week', and numerous other publications are CFR members. The organization's members also dominate the academic world, top corporations, the huge tax-exempt foundations, labor unions, the military, and just about every segment of American life," write Jack Newell and Devvy Kidd.
The "pressure from above" mentioned by Rarick is being used to silence influential critics of the concept of a one-world dictatorship now in motion.
It is, however, too late for the control freaks and one-worlders to squash the opposition. Google's YouTube may have swept The Alex Jones into the memory hole, but this will not prevent the message from reaching millions of people who now know the New World Order is determined to reduce the planet to a slave labor gulag run by the international bankers and their minions.
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Newswars Redirect
Eminem Invokes Vegas Mass Shooter in New Anti-Gun Anthem
WATCH: Sheriff's Deputy Vows To Defy 'Unconstitutional' Gun Control
Middle Schooler Threatened With Suspension Over 'Virginity Rocks' Sweatshirt
Eminem gets slammed for lyric on bombing of Ariana Grande's Manchester concert
US Begins Airport Screenings After Second Patient With SARS-Like Pneumonia Dies In China


text:
Independence Blue Cross Announces Big Drops in Opioid Prescriptions and Use Among Members
A new report from the Blue Cross Blue Shield Association shows a dramatic reduction in opioid use and prescriptions among network members. Still, the report recommends continued emphasis on the crisis.
By Fabiola Cineas·	 7/13/2018, 12:40 p.m.
Charles Wollertz | iStock
Independence Blue Cross says it's making headway in fighting the opioid crisis. The insurer's efforts over the last four years have led to a dramatic reduction in opioid use, prescriptions and abuse among members, according to a national Health of America report by the Blue Cross Blue Shield Association released on Thursday.
Since 2014, 45,000 fewer Blue Cross Blue Shield members are using opioids — a 45 percent reduction. The group is also reporting a 35 percent reduction in opioid prescriptions (100,000 total) and an 18 percent reduction in the morphine equivalent dose.
In the Philadelphia region specifically, opioid prescriptions among members decreased by more than 30 percent between 2013 and 2017, according to the report. Nationally, opioid prescriptions among Blue Cross Blue Shield members dropped by 29 percent during that same period.
The report notes that there's a significant variation among states. Thirty-four states had higher reductions than the national figure. Massachusetts leads with a 51 percent reduction in the total number of opioid medications filled by commercially insured Blue Cross Blue Shield members.
Independence says a change in physician prescribing habits is one reason for the decrease in prescriptions. The insurer continues to share the Centers for Disease Control opioid prescribing guidelines with its network providers and has given detailed reports to more than 1,000 prescribing doctors about members who exceeded the recommended morphine equivalent dose.
Last summer the insurer also began restricting first-time, low-dose opioid prescriptions to a five-day supply limit. Patients with cancer or terminal illnesses were exempt from the rule.
IBX says the change, which was designed to limit unnecessary harm from opioid use, resulted in a "substantial reduction" in use and prescriptions. During the last six months of 2017, the number of members using opioids dropped 22 percent and the number of prescriptions dropped 26 percent compared to that same time period in 2016.
The report concluded that continued emphasis on the opioid crisis is necessary to further reduce opioid consumption and dependency in the U.S. While progress has been made, there were 241,900 Blue Cross Blue Shield members diagnosed with opioid use disorder in 2017.
independence blue cross
Fabiola Cineas	Business Editor @fabiolacineas
fcineas@phillymag.com
The Path to a Cure: Temple HIV Treatment Milestone Was 5 Years in the Making


text:
Bridges, March 20, 2020
FROM THE LCWR PRESIDENCY
A Call to Spiritual Bonding by Elise D. García, OP - LCWR President-Elect
As I write this column, the disruptive impact of the COVID-19 pandemic is rocking our nation and the world. Social distancing is the catchword. We leaders of religious institutes, along with leaders of governments, schools, parishes, businesses, civic organizations, industries, and nonprofits, are challenged with making daily, if not hourly, determinations about the breadth of its application as a proactive form of quarantine.
That this time of global sickness and quarantine has come during Lent gives us cause for deep spiritual reflection. The term "quarantine" comes from the Italian quarantena – meaning a 40-day period – and it originates from the days of the Black Death in the 1300s. As we are called to engage in social distancing for the common good of all, our 40-day Lenten journey this year includes the sacrifice of missing significant gatherings, weddings, birthdays, funerals, liturgies, and the daily social interactions we so take for granted. Concerns about the impact of isolation heighten awareness of the precious gift of simply being with one another.
All of us in leadership are acutely aware that our motherhouses are full of elderly sisters who comprise the population most vulnerable to the ravages of this novel disease – and we are all taking every precaution to protect them and the larger communities we serve. These very same women, however, are also among the world's most resilient spiritual practitioners!
As we women religious take the prudent measures this global pandemic requires, perhaps we might also take a leadership role in countering the ill effects of social distancing by advancing the practice of spiritual bonding. Our motherhouses are powerhouses of prayer and presence. How might we join together to find ways of uniting the human spirit in faith, love, and solidarity among ourselves and others across the globe as we all face this common viral threat?
We are already seeing marvelous examples of this: As Italy moved into complete lockdown, Italians spontaneously came out on their balconies to join in song, banging pots and pans in expressions of gratitude to healthcare workers. To raise morale in their beleaguered nation, Iranian healthcare workers tweeted videotapes of themselves dancing in full protective gear.
What witness to the presence of God in the midst of all this suffering might we women religious offer at this time? How might our prayers and intentions be joined across congregations for the common good of the whole Earth community to help lift the spirits of a people, especially in the wake of closed churches, synagogues, mosques, and other places of worship? What would happen if elder Catholic sisters, among those most susceptible to fatality from exposure to COVID-19, were to unleash the power of their lifetime of prayer and contemplative practice to hold the safety and protection of all peoples across the world as a sacred intention?
How might a call to spiritual bonding witness to our oneness as a global community, helping to allay fears and touch the isolation of social distancing?
The International Union of Superiors General (UISG) has called upon all women religious throughout the planet to spend Sunday, March 22 as a Day of Worldwide Solidarity and Prayer. "This is a special time for prayer and for witness through practical solidarity and awareness of our responsibility to care for one another....," said UISG president Jolanta Kafka, RMI. "We therefore invite all the member congregations of UISG to make March 22 a day of worldwide solidarity and prayer especially for all those directly affected."
LCWR encourages all leaders to ask their members to join intentionally their own prayer with Catholic sisters throughout the world who will also be praying for those directly impacted by this crisis. Through the mystery of God, may this action of solidarity contribute in some way to an increase in healing, compassion, and love throughout the planet.
(Attached to the Bridges email is an excerpt from the LCWR Newsletter for April, that you'll also want to read.)
COVID-19, LCWR
Bridges, April 16, 2021
Bridges, August 7, 2020
Bridges, May 22, 2020
Bridges, May 1, 2020


text:
Trump Approval Rating Hits 45 Percent
By Jack Phillips
December 8, 2017US
President Donald Trump greets guests while holding his granddaughter Chloe Sophia Trump after arriving at the White House in Washington on Dec. 2, 2017. (Samira Bouaou/The Epoch Times)
President Donald Trump's approval rating increased to 45 percent in the first week of December.
According to a Morning Consult/Politico poll released on Dec. 6, Trump's support was especially strong among religious groups, notably Christians (52 percent), with 60 percent of Evangelicals, 57 percent of Protestants, and 47 percent of Roman Catholics giving him the thumbs up.
The poll was conducted between Dec. 1 and Dec. 3 among a national sample of 1997 voters.
The poll also showed that 48 percent of registered voters trust Republicans in Congress to fix the economy. Only 32 percent of them said they trust Democrats to do the same.
Senate Republicans passed a tax bill last week aiming to increase economic growth by lowering the corporate tax rate from 35 percent to 20 percent.
Last month the House passed its version of the tax bill. House and Senate Republicans are now negotiating a final version of the bill that both groups will support.
The bills received no favorable votes from Democrats in either the House or the Senate.
Since coming to office in January, Trump has delivered on many of his campaign promises.
The ISIS terrorist group has been severely weakened and is on the run following the fall of its self-proclaimed caliphate in Raqqa, Syria.
The economy has improved significantly, reaching a 3 percent GDP growth in Q3, compared to a 1.6 percent average for 2016. Unemployment had dropped to 4.1 percent.
Stock markets have added over $5 trillion in value. Illegal crossings over the southern border under the new administration have dropped by 60 percent.
If you enjoyed reading this article, support our independent journalism by sharing it on social media.
From The Epoch Times
EU Ministers Seek Trump-Style Border Walls Amid Spike in Illegal Border Crossings
San Francisco Will Appeal Court Injunction In Homeless Encampment Lawsuit
FDA Advisers Back COVID-19 Vaccine Pivot in Move Toward Annual Shot
US Military Kills Major ISIS Figure Bilal al-Sudani, 10 Other ISIS Terrorists in Somalia
First Officer: Alex Murdaugh Didn't Cry Over Dead Wife and Son
Nanjing Sees 6-Fold Increase in COVID Deaths: Report
Biden Touts State of Economy, Bashes 'MAGA Republicans' in Virginia Union Hall Speech
Church Torn Down in China's Zhejiang Province


So I was sorting through my org-mode files and I found a little snippet of code that I had lying around. I've had a problem with shell scripting for a while. I use bash a lot, and I've written a few functions, and procedural scripts that I've found useful in my travels, but anything that requires "logic," often escapes me in tragic and epic ways.
It works as a one liner, but it works. I think previous attempts have left out crucial semi-colons or the do and done statements. No clue. Baby steps folks.


text:
Epworth Eastern is a finalist for an Australian Private Hospitals Association award for its driving program
Anthony Mallamace is giving his dad and other patients free rides to Epworth Eastern through its volunteer driver program
A Doncaster man with a decades-long involvement as a patient with Epworth Eastern is giving back as a volunteer driver.
Anthony Mallamace, 54, has a deep connection with the Box Hill hospital where he and his father have been frequent visitors over the years.
He's received treatment at the hospital for Crohn's disease, which he has had for 30 years, and the heart attack he suffered in 2010.
His association with the hospital continued when he became the carer — and driver — for his father Joe, who has regular dialysis appointments.
"Basically dad's dialysis drew me here, but to understand the clinical side of it and what he goes through is more of a factor," he said.
"I wanted to help the hospital in any way for the support they give to Dad, plus we've made a few friends here."
Mr Mallamace signed up for the hospital's volunteer patient driver program two-and-a-half years ago.
The service is funded by the hospital and gives patients free lifts from their homes to appointments.
Along with his dad, Mr Mallamace has more than 10 regulars he interacts with in his two days of volunteering every week.
There's no loud music in the car — instead he and the patients have a chat to get their problems off their minds.
"We have a good conversation and a chat, everyone enjoys that moment in time," he said.
"It gives everyone time out from thinking about what they're going to face."
Mr Mallamace said being a volunteer driver also gave him great personal satisfaction.
"At the end of the day, you've achieved something and you don't expect to get anything back, it's as if you've kicked a winning goal."
Epworth Eastern began its driver program in 2017 and now has more than 40 volunteers offering their time in various departments at the hospital.
It operates six days a week and has been nominated for an Australian Private Hospitals Association award later this year.
People keen to join the driver program can express their interest on the 'Volunteering' page at epworth.org.au
Courtesy: Manningham Leader
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