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Home > Scandals > The Wendy Williams Show
Wendy's Comeback! 'Happy' Williams To 'Focus On Her Career' After Dumping Husband
Source: Paras Griffin/Getty Images
Apr. 12 2019, Published 7:34 p.m. ET
Everyone loves a good comeback story — and Wendy Williams is no exception!
Just one day after the 54-year-old talk show host filed for divorce from her husband of 21 years, Kevin Hunter, RadarOnline.com exclusively learned she's "happy," and "focusing on her career."
According to a friend of Williams, "It's like the hills are finally alive with the sound of music again for her. When we spoke after she filed she actually sounded happy! And we are happy for her!"
As fans know, Williams' tumultuous marriage to Hunter, 46 — who also served as her manager and talent agent — was plagued with infidelity.
In her 2001 memoir Wendy's Got The Heat, she shared with fans that her husband cheated on her during the birth of their son.
For the past several years, Hunter has been accused of having an affair with his alleged mistress Sharina Hudson. In a report published by Us Weekly, the outlet stated that Hunter was spotted buying groceries for Hudson — who allegedly gave birth on March 25 to a child that is believed to be Hunter's. Although Williams told fans to "not believe the hype," the source told RadarOnline.com exclusively it's too late for that!
"Kevin was dead weight, and she will be okay in the end. She may not even realize this yet, but this is the best thing for her. He needed to be out of the picture for so many reasons and now he finally is. Her friends will continue to support her," the source told RadarOnline.com.
For the past several months, Williams' erratic behavior has caused great concern for her fans. On January 18, after passing out while filming her hit talk show, Williams announced that she was going on hiatus to deal with health complications.
The Wendy Williams Show
Baby Bombshell! Wendy Williams Confirms Cheater Ex Has A Secret Daughter
Wendy Williams 'Is Having Second Thoughts About Divorce' From Husband Kevin Hunter
Wendy Williams & Husband Kevin Hunter Divorcing After Rehab & Cheating Scandal
Williams returned to the air on March 4 and, on her comeback episode, insisted that everything was fine between her and Hunter!
"Marriages are not easy – and don't ask me about mine until you see this gone. It ain't going anywhere, not in this lifetime. He is my best friend, my lover, he's all this and he's all that. I know what you've been saying and I know what the streets have been talking about," Williams said at the time.
On March 10, Williams got honest with her fans and admitted that she had moved out of the home she shared with her husband and into a sober living facility in Queens, New York — where she was being treated for an addiction to alcohol and prescription pills.
Just two weeks later, on March 25, the fallen talk show queen was spotted without her wedding ring when she was rushed to a hospital following a relapse on alcohol.
Wendy Williams Nemesis Janet Hubert Takes Kevin's Side In Ugly Divorce: 'He's Free!'
Wendy Williams' TV Show Staff 'Thrilled' She Filed For Divorce From Cheating Husband Kevin Hunter


Today's the day NASA remembers the tragedies and the lives lost in the space program. Three big ones come to mind: the Apollo 1 in 1967, the Challenger explosion in 1986, and the breaking apart of the Shuttle Columbia in 2003. It's one of those things where you remember "where you were when it happened." What about you? Where were you?


Endeavour 'gouged' by a piece of ice shortly after take-off.
An analysis of images taken on Wednesday during lift-off in Cape Canaveral, in Florida, showed that the shuttle's underbelly was hit by a piece of ice, Shannon said.
"What this means, I don't know at this point," he said.
The possible damage was detected on Friday after ISS crew members photographed the shuttle's underside during its approach to the station.
On Sunday, astronauts are due to use a camera attached to a robotic arm to closely inspect the area of concern, Shannon said.
Astronauts will carry out a space walk to patch up the hole if Nasa decides the gash threatens Endeavour's safety during its return to Earth.
Shannon said that other shuttles have returned safely with worse damage.
"In the past, we didn't even know we had damage and we flew back home," he said.
But since the Columbia shuttle crash in February 2003, Nasa has carefully inspected protective thermal tiles.
Columbia's heat shield was pierced by a piece of insulating foam that from its external fuel tank, causing the shuttle to catch fire as it re-entered the Earth's atmosphere.
The shuttle exploded killing seven astronauts.


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CHSO Presents: Cinema Musicale – A Night at the Movies
The Claflin Hill Symphony Orchestra (CHSO) will present the final concert of its "Crystal Anniversary Season" on Saturday, April 25, at 7:30 p.m. at the Milford Town Hall Grand Ballroom and audience members can be part of the excitement. "We invite our concertgoers to... Read more
Three Dog Night at Indian Ranch
Legendary music icons Three Dog Night return to Indian Ranch Sunday, July 26 at 2:00 P.M. Celebrating their 4th decade, Three Dog Night's hits wind through the fabric of pop culture today whether they are heard on the radio. Three Dog Night had 21 consecutive Top 40... Read more.
LiveARTS Presents The LiveARTS String Quartet
LiveARTS' season's climax and finale is presented by their own LiveARTS String Quartet. Six seasons ago LiveARTS learned about a group of four immensely talented string players who had been playing together but had not yet given a public performance as an ensemble. They... Read more.
04/04/2015 - 11:00:24 AM
Live and Local Music Hop - Satuday April 4th
By WMRC's Ray Auger - So much great talent in one local music scene! On any given Friday or Saturday night (and even Thursdays) you can catch 3 or 4 great shows if you time it correctly and hit the right venues at the right time. Here's a Live and Local Music Hop... Read more.
Live and Local Music Hop - Friday April 3rd
The Ultimate LMA Nominee Companion
On April 1st we announced the nominees for the 2015 WMRC Local Music Awards! The winners will be announced and honored at Liz's Diamond Bar and Grille, winner of the 2014 Best Local Music Venue, on Sunday May 17th. Putting together the list of nominees, with the help... Read more.
The 2015 WMRC Local Music Awards is May 17th!
The stage is set for this year's WMRC Local Music Awards! On May 17th hundreds of musicians, fans and local music supporters will gather at Liz's Diamond Bar and Grille in Hopedale to honor, celebrate and relish all that The Greater Milford Area Local Music Scene offers... Read more.
The Live and Local Music Hop for Sat (3/28)
The Live and Local Music Hop - Friday Night (3/27)
Paternull Benefit for Hopedale Youth Baseball
The Hopedale Youth Baseball 2015 Cooperstown Team would like to invite members of the community age 21+ to join us Saturday, April 4, at Scioli's Pizza Bar, for a concert with Paternull. We'll have food and a cash bar available, along with silent auction items... Read more.
Ten Questions With Tony Soul
Tony Soul is back after a 42 year musical absence! His band, The Tony Soul Project, is bringing the blues to the local area. Ray Auger talks to Tony about jazz, The Local Music Social, lack of free time and more... Read more.
The Live and Local Music Hop - Saturday Night
The Live and Local Music Hop - Friday Night
So much great talent in one local music scene! On any given Friday or Saturday night (and even Thursdays) you can catch 3 or 4 great shows if you time it correctly and hit the right venues at the right time. Here's a Live and Local Music Hop suggestion if you feel like... Read more.
We Were Astronauts to Perform at Local MS Benefit
This Saturday night, March 21st, We Were Astronauts take the "stage" of The Tradesman on Route 140 in Milford to raise lots of money for a cause that affects many of us. Whether it's you, me, a family member, a friend or a friend of a friend, Multiple Sclerosis, disease... Read more.
Jonathan Edwards at Circle of Friends
Since 1971, Jonathan has released 15 albums, including Blue Ridge, his standard-setting collaboration with bluegrass favorites the Seldom Scene and Little Hands, his collection of children's songs, which was honored with a National Library Association award. He measures... Read more.
CHSO Presents Fire and Ice
The Claflin Hill Symphony Orchestra will present its annual family matinee concert on Sunday, March twenty second at three p.m. in the Grand Ball Room of the Milford Town Hall. The concert, titled "Fire and ice" is designed for families with children of all ages and also... Read more.
NECMC Jamboree
The New England Country Music Club's next Jamboree will be held Sunday March 15th at the Uxbridge VFW Hall on Route 16th. Dancing from 1 to 5pm. $5 for members. $7 for non-members. Doors open at 12:30. The band Branded will be entertaining! Read more.
Ten Questions With Tommy Pile
Tommy Pile has been playing out in the local music scene for quite some time now. His new original project, Bad Men, are getting ready to release their new CD. Ray Auger talks to Tommy about Kickstarter, funeral songs, the joy of synth and more... Read more.
2015 WMRC Local Music Awards
It's that time again! Time to celebrate our local music scene! Join WMRC, Liz's Diamond Bar & Grille, Three Olives Vodka and Allen Engineering on May 17th for a night of honors, live music and fun! We'll have a VIP Suite for our nominees and a few lucky winners... Read more.
Mark Erelli in Live Franklin
Acclaimed folk singer Mark Erelli has tackled everything from western swing and protest songs to lullabies and murder ballads. This will be a CD release concert for his latest CD, "Milltowns," a tribute to Bill Morrissey. He will be joined by Richard Gates. Surly Temple... Read more.
The New England Tenors in Hopedale
The New England Tenors will perform a special concert at the Union Church in Hopedale, Mass. on Sunday, March 8th from 2pm to 4pm. The Tenors will be joined on stage by the Greater Milford Community Chorus under the direction of Daniel Zabinski with piano accompanist... Read more.
Claflin Hill's A Chorus Line-Up: Opera to Broadway
The Claflin Hill Symphony Orchestra continues the celebration of its fifteenth Anniversary Season, "The Crystal Anniversary Season" with "A Chorus Line-Up – Opera to Broadway" on Saturday, March 7, 2015, at seven thirty p.m. in the orchestra's beautiful home venue... Read more.
Ten Questions With Gay Barboza
Gay Barboza could be considered one of the hardest working local musicians in our area... and one of the most talented! Ray Auger asks Gay about music, life and inspiration. Check out Ten Questions with Gay Barboza. Read more.
Original Music is Alive and Well in Small Town, MA!
By WMRC's Ray Auger - In a small town area like ours it's typically the cover band that thrives in the bars and clubs, attracting the masses who crave to dance, tap their feet or bang their heads to songs they all know and love. But we are starting to see a trend in... Read more.
The End of Guitar Center
This is an obituary for Guitar Center, a chain of big box musical instrument stores that was captured and infected by private equity during a national trend of greed and reckless expansionism in the late-1990s and early-2000s. The company started as a Los Angeles organ... Read more.
Homegrown Original Music Showcase
The Local Lowdown presents The Homegrown Original Music Showcase featuring Sheez Late Acoustic, Grand Evolution, Jennifer Tefft Band and Born Without Bones. Read more.
The Local Lowdown for the Week of January 25th
WMRC's Local Lowdown is a collection of what's happening in the local music scene in our area. Live and local bands playing at local venues. Support Local Music! Read more.
Ten Questions With Rich Teter
Rich Teter has been playing music in the local area for quite some time now. Ray Auger asked Rich about his band Teter Todders, Dave Grohl and more. Check out this weeks Ten Questions With... Read more.
Milford TV Presents The Coffee House Concert Series
WMRC's Ray Auger partners up with Milford TV to introduce the local area's most talented singer/songwriters with this monthly series that airs on Milford TV. The Coffee House Concert Series feature three artists taking turns performing their music and telling the stories... Read more.
Living For The Weekend Live Performances
Listen to Living For The Weekend on WMRC Fridays at noon. Ray Auger talks to a variety of people about events and happenings in the local area. Most shows feature musicians performing acoustic music and promoting their local shows. Read more.
Ten Questions With Derek Walker
Milford's Derek Walker has been playing music in the local area for 23 years and now he's saying goodbye to his hometown. Ray Auger asked Derek about his band Fourcast, Austin, TX and more. Check out this weeks Ten Questions With... Read more.
We Were Astronauts Release EP
There's an up and coming band living in our midst. A band that, if you heard on the radio today, would fit right in with the indie rock likes of Kings of Leon or NeedtoBreathe. One radio hit would blend into a We Were Astronauts new release and seamlessly transition... Read more.
Ten Questions With Chris Ross
Medway's Chris Ross is not only an accomplished musician but he's also the coach of the Medway High School Boy's Hockey Team. Ray Auger asked Chris about hockey, music and more. Check out this weeks Ten Questions With... Read more.
Jim Ligor Releases New Single on iTunes
James Thomas Ligor's smooth energetic vocals pay homage to not only the eloquent confessional singer-songwriter movement of the 1970's but also draw from the energetic and anthemic rock explosion of the modern country scene... Read more.
Local Music Spotlight - If We Go At All
Hailing from Milford, MA. Culled from the parts of other local acts. If We Go At All is an original outfit creating indie rock for people who are interested in music, and being liberated by it. Influenced by many, similar to few... Read more.
Local Music Spotlight - Jenn Tefft
Jennifer Tefft is a fired up, energizing presence who pulls earthy music from its roots and breathes fresh, soulful, rock and roll life into them. Her music combines intense rhythms with melancholy textures and haunting vocals that wind easily from darkly... Read more.
Q & A With Caitlin Arcand
WMRC's Ray Auger talks with local musician Caitlin Arcand about her music and her Vans sneakers! Read more.
2014 WMRC Local Music Award Winners
The 2014 WMRC Local Music Awards were Sunday May 18th at PiNZ in Milford. 11 bands, 30 awards and it was all FREE! Hundreds came out to celebrate local music with some of the best musicians in the New England area. It all started with a red carpet party... Read more.
MyFM in the Morning's Lowdown is

redpajama_set_name: RedPajamaCommonCrawl


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New Zealand Cricket Allows Players To Choose Between The IPL And The Pakistan Tour
New Zealand Cricket (NZC) has allowed its players to choose between featuring in the historic Pakistan tour or the 16th edition of the Indian Premier League (IPL) next year. The Kiwis will visit Pakistan in two phases – in December 2022-January 2023, followed by April-May 2023 to play in all formats.
In December 2022 and January 2023, New Zealand will travel to Pakistan for the first leg of the ICC World Test Championship, which consists of two Test matches. As both teams strive for direct qualification in the 50-over tournament next year, the tourists will also take part in three World Cup Super League matches.
New Zealand team. Photo- ICC
From April 13 to May 7, the second leg of the tour will feature five ODIs and just as many T20Is and will conflict with the lucrative Indian league. Players like Kane Williamson, Trent Boult, Lockie Ferguson, and Mitchell Santner will probably need to make a choice.
"As of our understanding, our full-strength side will go to Pakistan. I haven't talked to players and their associations further in this regard. But, players will be allowed to play in IPL. They will be free to choose between IPL and Pakistan tour," David White said.
New Zealand Team (Credits: Twitter)
"Our delegation visited Pakistan earlier this year. We are in contact with the embassy and our government about this tour," David White, CEO of NZC, stated to New Zealand media
Pakistan is a team that is formidable in all formats: New Zealand captain Kane Williamson
Kane Williamson, the captain of the Black Caps, expressed his excitement to play in Pakistan and predicted that the visitors would be a formidable opponent. In a video posted by Pakistan Cricket on Twitter, the right-handed batter said:
"It's really exciting playing cricket back in Pakistan. Such rich cricketing history, so many incredible matches that have been played here, and we are looking forward to that experience."
Kane Williamson (Image Credits- Twitter)
"Pakistan is a team that is formidable in all formats, so we know it's a tough task, but it's a challenge we look forward to. As a team, they are always well-balanced. They have produced a lot of fast bowlers and have the batting to go with it all. Their captain Babar Azam is the top in the world."
The current tri-nation series between the two teams also includes Bangladesh. In the series finale, Pakistan and New Zealand will likely face off.
Also Read: Sourav Ganguly Will Not Be Nominated For The ICC Chair By BCCI – Reports
Cole lauds 'picture perfect' Chelsea star set to become club's highest earner
'Arsenal can't compete' for Bellingham as Lescott claim is rubbished – five clubs 'really want him'


I started working when I was 12 or 13 years old. I remember rolling up newspapers for my paper route, rubber banding them and riding my pink, banana seat bike all around the neighborhood, tossing newspapers at each front porch.
At 15, I started working at a pizza place and I worked there all through high school. I worked every summer. I worked and worked and worked some more.
After having both children, I worked full time without a second thought. I was used to working and juggling life around it. Then six years ago, we decided to move cities and knew it would be the perfect time to take a step back and be home with the children. These years are short (or so I hear) and we both wanted a simpler life for ourselves and our children.
Now, fast forward six years and the kids are older and are both in school. Whew – free and clear! I was offered a part-time job as a baker and snatched it up. I couldn't wait to get back into the working world. Co-workers! Paychecks! I was also looking forward to the ability to easily answer the question "so what do you do?" Stay-at-home mom always seemed to fall so flat. It sounds boring. It sounds like under-achieving. It sounds so privileged.
But then we were back to the daily juggling. Our simpler life went out the window. After working for a year, my body was telling me no, it was time to say good-bye to the baker position and return to the stay-at-home mom one.
That brings me back to here.
Raising humans is a monumental task, yet it is made up of a million smaller ones. Packing lunches, laundry, homework, bedtime stories and play dates – all add up to what we hope are responsible adults who are ready to take on the challenges of this world. Yet, sometimes its hard to see the forest for the trees. The mundane tasks seems so – mundane.
I hadn't realized how much my self worth was attached to my employment until I stopped working. It is hard for me to remember that in fact, self worth comes from me just being me.
In light of this, I'm trying to remember that me just being me is enough. I don't have to earn my keep, so to speak. I do plenty. I can plan coffee dates with friends and indulge in hobbies. I can spend part of my child free time on things that enrich my life as an individual. Volunteer, read, and of course, bake.
Now, with this extra lease on life, I decided it was time to work on some tasty new pancakes. Blueberry pancakes have never really been a family favorite. A couple years ago, our youngest was watching Daniel Tiger on PBS and they made strawberry pancakes on the episode. He immediately asked to make them and so we did. This time around, I embellished them with a zing of lemon and a powdered sugar for the topping.
Whisk together the flours, sugar, baking powder, salt and lemon zest in a medium bowl. In another bowl (I use a large measuring cup) combine the milk, butter and vanilla. Pour milk mixture into flour mixture and combine with a spatula until just combined. Gently mix in strawberries. Pre-heat a griddle to 350 degrees. Spray griddle with cooking spray and ladle 1/4 cup mixture unto griddle. Cook until lightly golden on the bottom (1-2 minutes) and then flip. Press the pancake down gently. Cook for another 1-2 minutes or until both sides are golden brown and the middle is cooked through.
I test the middle of the pancake by gently pressing the side of the spatula into the pancake and if it comes out clean, then I know the middle is cooked. Serve with a bit of butter and powdered sugar.
I love every bit of this and can relate to a lot of it. I look forward to more recipes as you find your groove again with more time on your hands.
Sometimes it just feels good to acknowledge the struggle and to know that there probably isn't a parent out there that doesn't feel it too. The pull between identities and the conflict between the people we want to be vs. the people we are. I love seeing all your photography and reading your posts. Keep it up!


At a facility for irradiating traditional Chinese medicine, five male workers entered the irradiation room and were exposed to the cobalt-60 source. The workers were exposed from 5-15 minutes each, about 0.8-1.5 meters from the source. They developed nausea and vomiting about 30 minutes later, exhibiting facial blushing, blepharal hyperemia, and drunken appearance. All five were transferred to a Beijing hospital 14 hours after exposure. Two victims (doses 1240 and 340 rad) developed acute gastrointestinal radiation sickness with severe bone marrow damage; the other three (doses 250, 220, and 210 rads) developed moderate bone marrow radiation sickness.
Yao, B., Y. Li, G. Liu, M. Guo, J. Bai, Q. Man, L. Qiu, and H. Ai, 2013, "Estimation of the biological dose received by five victims of a radiation accident using three different cytogenetic tools," Mutation Research, 751:66-72.
Ying, C., D. Jie, Z. Xueqing, L. Qingliang, Z. Zhiping, and T. Rong, 15 Oct. 2012, "Biological dose estimation in five victims of a cobalt source accident and cytogenetic follow-up observation after one years," European Radiation Research 2012, on line [http://www.iss.infn.it/err2012/satellite/program/POSTER/Chen_ISCA10.pdf].
© 2013 by Wm. Robert Johnston.
Last modified 26 June 2013.


Charalambos Poullis, Leila Sujir and Santiago Tavera presented their research and latest projects September 17, 2016 at the Entertainment Technology Summit part of the Festival International du Film Canada-China 2016 at Concordia University.
The Entertainment Technology (ET) Summit will be crucial in constructing a platform of mutual academic learning and communication in the field of film production. Film technology specialists will discuss and exchange thoughts on cutting-edge film technology. CCIFF will also invite international keynote speakers and well-known Canadian and Chinese film companies to participate in the summit. The ET Summit will offer an informative and dynamic atmosphere and opportunities for networking and discovering new technology.
The ET Summit will be held on September 17, 2016, at 9:00am. Film technology specialists will discuss multimedia technology and post-production skills, and brainstorm with the other film producers on near and long-term possibilities for collaboration. CCIFF will also invite famous Canadian and Chinese film and entertainment companies to participate, providing the summit with an informative and dynamic atmosphere and offer opportunity for networking and forming co-production initiatives.


Alibaba Group Holdings Limited has acquired an online translation services provider 365Fanyi, which is backed by Zhen Fund and China Broadband Capital (CBC), according to the company's website indicating its ownership by Alibaba.
The acquisition of 365Fanyi, which has 500 specialized translators and interpreters, will help Alibaba as the Internet giant focuses on international expansion going forward.
Financial details of the deal are not disclosed.


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\section{Introduction}
\label{sec:intro}

Gamma-ray binaries are a small, but growing class of high mass binary systems, which are characterized by non-thermal emission which peaks in the gamma-ray regime \citep[$>1$\,MeV, see e.g.][]{dubus13}. To date there are eight known systems,
all of which consist of an O or B types star and a compact object in the mass range of a neutron star or black hole \citep[e.g.][]{ chernyakova19, corbet19, dubus13}. While the compact object is, for most systems, not directly detected, it is most likely a young, non-accreting radio pulsar and the non-thermal emission is produced in the shock that forms between the pulsar and stellar winds.  This is known to be the case for two systems, namely PSR~B1259-63 and PSR~J2032+4127, where pulsed emission has been detected \citep{johnston92,fermipulsars09}.

Shortly after the \textit{Fermi} discovery of PSR~J2032+4127\xspace as a $\approx143$\,ms gamma-ray pulsar, it was also detected to be a pulsar at radio frequencies  \citep{Camilo09}. The source lies close to the extended TeV HEGRA source, TeV J2032+4130  \citep{hegra05}, and it was proposed that this was a pulsar wind nebula powered by PSR~J2032+4127\xspace \citep{aliu14}. However, while PSR~J2032+4127\xspace was first thought to be an isolated pulsar \citep{Camilo09}, further radio observations demonstrated a rapid increase in its observed spin-down rate, which was interpreted as evidence that the pulsar is a member of a highly-eccentric binary system, where the optical companion is a $\sim$ 15 M$_{\sun}$ Be star, MT91 213 \citep{lyne15}. PSR~J2032+4127\xspace thus turned out to be similar to PSR~B1259-63\xspace, where a 48\,ms pulsar is orbiting around a Be star, LS~2883, in an eccentric, 3.4 years orbit \citep[e.g.][]{johnston92}.

Further multi-wavelength monitoring of PSR~J2032+4127\xspace by \citet{ho17} refined the orbital period  to be in the range of $16\,000$ to $17670$ days, with an eccentricity of $e = 0.961$ (separation at periastron is $\alpha_{\rm per}\sim 1$\,au)  and found the  periastron passage would occur in November 2017. Subsequent observations around this period were in  good agreement with this prediction, and in this paper we adopt  $t_{\rm per}$=MJD 58069 as the date of the 2017 periastron.

\textit{Chandra} X-ray observations reported in \citet{ho17} demonstrated a strong rise in the  source brightness;  PSR~J2032+4127\xspace was about 20 times brighter in 2016 than it was in 2010, and about 70 times brighter than it was in 2004. This increase was interpreted as a result of the collision between pulsar and Be star winds. Smoothed-particle hydrodynamics (SPH) modelling of the winds interaction presented in \cite{coe19} demonstrates the deformation and even partial destruction of the Be star disc at some orbital phases.

Modelling of the source suggested that around periastron the binary should be detectable at TeV energies \citep{bednarek18,takata17} and PSR~J2032+4127\xspace was subsequently detected at TeV gamma-ray energies by the VERITAS and MAGIC telescopes as a point-like source \citep{psrj_tev}. The TeV light curve peaked at periastron (followed by a short dip a few days later). The observations also showed that during the brightest period (at periastron) the spectrum is best fit by a power-law but when the source was fainter during the 2017 observations (before periastron) a power-law with an exponential cut-off is favoured.

Long term observations of the Be optical companion, MT91 213, have shown the star has demonstrated strong variability showing periods of marked changes in the emission lines. Earlier observations (during 2012 and 2013) showed the stellar spectrum changed between a normal B star to a Be star \citep{salas13} while \citet{ho17} showed that the H\,$\alpha$ equivalent width varied from $W_\lambda = -13.2$\,\AA{} (in 2009) down to $W_\lambda \approx -4$\,\AA{} (in 2014-early 2016). It subsequently showed a rise to   $W_\lambda \approx -10$\,\AA{} before decreasing again over a $\sim200$ day period in the second half of 2016 \citep{ho17,coe19}. Around $\sim200$\,d before periastron, it is seen the equivalent width smoothly decreases towards periastron \citep{coe19,kolka17,roucoescorial19}.

In this paper we present results of intensive optical observations of PSR~J2032+4127\xspace with the Nordic Optical Telescope (NOT) starting approximately 100 days before periastron and lasting up to 50 days after it. These observations were complemented by X-ray (\textit{Swift}/XRT\xspace, \textit{NuSTAR}\xspace) and GeV (\textit{Fermi}/LAT\xspace) monitoring. Joint analysis of the evolution of the parameters of the H\,$\alpha$ line and the broadband (X-ray to TeV) spectral shape allow us to propose a model linking the observed emission to the interaction of the pulsar and Be-star winds.

\section{Data analysis}
\label{sec:data_analysis}
\subsection{\textit{Fermi}/LAT\xspace data analysis}
\label{sec:lat_data_analysis}
\textit{Fermi}/LAT\xspace data selected for the analysis presented in this paper cover more than 11 years (Aug. 2008 to Dec. 2019). We used the latest available \texttt{fermitools}  with P8\_R3 response functions (\texttt{CLEAN} photon class).\footnote{See \href{https://fermi.gsfc.nasa.gov/ssc/data/analysis/documentation/Cicerone/Cicerone_LAT_IRFs/c }{description of \textit{Fermi}/LAT\xspace response functions} }

To extract the spectra we performed the standard binned likelihood analysis of a region around PSR~J2032+4127\xspace. The spectral analysis is based on the fitting of the spatial/spectral model of the sky region around the source of interest to the data. The region-of-interest considered in the analysis is a circle with a radius of 18 degrees around PSR~J2032+4127\xspace.  The model of the region included all sources from the 4FGL catalogue~\citep{lat_4fgl} as well as components for isotropic and galactic diffuse emissions given by the standard spatial/spectral templates \texttt{iso\_P8R3\_CLEAN\_V2.txt} and \texttt{gll\_iem\_v07.fits}.

The spectral template for each 4FGL source in the region was selected according to the catalogue model. The normalizations of the sources were considered to be free parameters during the fitting procedure. Following the recommendation of the \textit{Fermi}/LAT\xspace collaboration, we performed our analysis with energy dispersion handling enabled.

\subsection{X-ray analysis}
\subsubsection{\textit{Swift}/XRT\xspace}
We accompanied the analysis of the source behaviour with historic \textit{Swift}/XRT\xspace observations of the region and the data from our recent \textit{Swift}/XRT\xspace monitoring campaign of PSR~J2032+4127\xspace. The data were reprocessed and analysed as suggested by the \textit{Swift}/XRT\xspace team\footnote{See e.g. the \href{https://swift.gsfc.nasa.gov/analysis/xrt_swguide_v1_2.pdf}{\textit{Swift}/XRT\xspace User's Guide}} with the \texttt{xrtpipeline v.0.13.4} and \texttt{heasoft v.6.22} software package. The spectral analysis of \textit{Swift}/XRT\xspace spectra was performed with \texttt{XSPEC v.12.9.1m}.
\subsubsection{\textit{NuSTAR}\xspace}
Three \textit{NuSTAR}\xspace observations of PSR~J2032+4127\xspace were performed on MJDs~57640, 58062 and 58078. The raw data were processed with the standard pipeline processing (HEASOFT v.6.22 with the NuSTAR subpackage v.1.8.0). We applied strict criteria for the exclusion of data taken in the South Atlantic Anomaly (SAA) and in the ``tentacle''-like region of higher background activity near part of the SAA. Level-two data products were produced with the \texttt{nupipeline} tool with the flags \texttt{SAAMODE=STRICT} and \texttt{TENTACLE=yes}. High-level spectral products (spectra, response matrices, and auxiliary response files) were extracted for a point source with the \texttt{nuproducts} routine. The corresponding background flux was derived from a ring-like (inner/outer radii of 39''/86'') region surrounding the source. The spectral analysis was performed in the energy range of $3-70$~keV.

\subsection{Optical spectroscopy}
High resolution (R=25000) spectra were taken with the NOT from MJD 57950 to 58120, covering almost the whole periastron passage of the target. The instrument used was the FIber-fed Echelle Spectrograph (FIES, Telting et al. 2014) in its lower resolution mode. The spectra cover the range from 3800 up to 8300~\AA. Exposure times were optimised for a good signal to noise ratio in the H\,$\alpha$ line region, therefore the signal to noise in the blue bands is very low. This, together with the emission lines filling in all visible Balmer lines in that range, made the blue part of the spectra unusable for spectral characterisation of the target. A summary of the spectra and signal to noise ratio around the H\,$\alpha$ line is shown in Table \ref{tab:opt1}. The history of H\,$\alpha$ profiles is shown in Fig.~\ref{fig:opt1}.

\begin{figure}
    \centering
    \includegraphics[width=0.99\columnwidth]{halpha_line_ev.pdf}
    \caption{Evolution of the H\,$\alpha$ line profile. Time runs upwards and from left to right. The difference (in days) between MJD and periastron passage (58069) is shown on the right side of each profile. Details for each spectrum are shown in Table \ref{tab:opt1}.}
    \label{fig:opt1}
\end{figure}

\begin{table}
    \centering
        \caption{Summary of H\,$\alpha$ parameters (namely, equivalent width in \AA, peak ratio and peak distance in km\,s$^{-1}$) are shown, together with the middle MJD time relative to periastron,  signal to noise (S/N) ratio and exposure time (EXP.). The given S/N  refers to the continuum around the H\,$\alpha$ line. }
    \label{tab:opt1}
    \begin{tabular}{@{}c@{}|c@{}|c@{}|c@{}|c@{}|c@{}|c@{}} \hline
    MJD & MJD-$T_{per}$ & S/N & EXP. & EW  & V/R & R-V  \\
        &             &     &   (ks) & (\AA)&   & (km~s$^{-1}$) \\
    \hline
57959.15 & -109.9 & 50 & 2.5 & -12.91$\pm$0.12 & 0.66$\pm$0.01 & 277$\pm$3	\\
57972.14 & -96.0 & 50  & 2.7 & -12.20$\pm$0.05 & 0.78$\pm$0.03 & 262$\pm$2      \\
57973.95 & -95.1 & 50  & 2.7 & -11.51$\pm$0.10 & 0.76$\pm$0.03 & 259$\pm$3      \\
57975.00 & -94.0 & 50 & 2.7 & -12.10$\pm$0.10 & 0.75$\pm$0.02 & 264$\pm$2      \\
57976.05 & -93.0 & 50 & 2.7 & -11.85$\pm$0.11 & 0.81$\pm$0.05 & 268$\pm$4      \\
57977.05 & -92.0 & 50 & 2.7 & -12.16$\pm$0.11 & 0.74$\pm$0.03 & 256$\pm$3      \\
58006.90 & -62.1 & 60 & 1.2 & -11.19$\pm$0.06 & 0.95$\pm$0.05 & 287$\pm$3      \\
58016.04 & -53.0 & 45 & 2.5 & -10.68$\pm$0.08 & 1.02$\pm$0.05 & 292$\pm$3      \\
58023.98 & -45.0 & 50 & 1.2 & -10.08$\pm$0.06 & 1.11$\pm$0.02 & 297$\pm$1      \\
58036.99 & -32.0 & 50 & 1.2 &  -8.47$\pm$0.06 & 1.12$\pm$0.03 & 298$\pm$4      \\
58048.00 & -21.0 & 25 & 1.2 &  -6.80$\pm$0.11 & 1.32$\pm$0.13 & 297$\pm$3      \\
58073.89 & 4.9 & 55 & 1.2  & -6.46$\pm$0.03 & 1.90$\pm$0.09 & 343$\pm$2      \\
58074.91 & 5.9 & 55 & 1.2  & -6.44$\pm$0.06 & 1.67$\pm$0.14 & 319.8$\pm$0.4	\\
58077.83 & 8.8 & 35 & 1.2  & -6.22$\pm$0.04 & 1.32$\pm$0.10 & 300$\pm$1	   \\
58087.81 & 18.8 & 65 & 1.2  & -6.21$\pm$0.07 & 2.48$\pm$0.27 & 327.5$\pm$0.5	\\
58088.93 & 19.9 & 55 & 1.2  & -6.54$\pm$0.06 & 2.40$\pm$0.09 & 338$\pm$1      \\
58092.84 & 23.8 & 60 & 1.2  & -7.02$\pm$0.05 & 1.92$\pm$0.27 & 330$\pm$1      \\
58093.80 & 24.8 & 40 & 1.2  & -7.04$\pm$0.07 & 1.72$\pm$0.11 & 324$\pm$1      \\
58107.85 & 38.9 & 20 & 1.2  & -8.26$\pm$0.05 & 1.71$\pm$0.14 & 290$\pm$4      \\
58109.81 & 40.8 & 50 & 1.2  & -9.52$\pm$0.06 & 1.67$\pm$0.05 & 305$\pm$1      \\
58110.89 & 41.9 & 30 & 1.2  & -9.13$\pm$0.11 & 1.74$\pm$0.16 & 312$\pm$3      \\
58115.82 & 46.8 & 35 & 1.2  & -10.14$\pm$0.05 & 1.61$\pm$0.13 & 297$\pm$1      \\
58118.81 & 49.8 & 40 & 1.2  & -10.45$\pm$0.08 & 1.67$\pm$0.03 & 292$\pm$1      \\ \hline
    \end{tabular}

\end{table}

In our observations the H\,$\alpha$ line profile is always double-peaked. The reddest peak is more prominent in our first spectrum, but that situation reverses in our last spectrum, where the bluest peak is the dominant one. This transition from one dominant peak to another is typical in Be star discs and is the observational footprint of a density wave within the disc \citep[see e.g.][]{telting94}.

We have performed a set of measurements of the  H\,$\alpha$ line which include the equivalent width (EW), the peak separation R-V, where R represents the red-most peak position and V the blue-most peak, and the ratio of peak fluxes V/R. In order to calculate the R-V distance in km\,s$^{-1}$, we have used the relationship $(R-V)=c(\lambda_R - \lambda_V)/\lambda_\alpha$, where $c$ is the speed of light and $\lambda_\alpha$ is the rest wavelength of the $H_\alpha$ line.  These parameters characterise the properties of the circumstellar discs around Be stars. The evolution in time of these three parameters can be seen in Fig.~\ref{fig:opt2}. Peak positions and fluxes have been obtained directly from the observed profile, by smoothing and finding each maximum when the slope of the line profile becomes null. All our measurements are in good agreement with those of \cite{coe19}.

We see a decreasing EW as the neutron star approached its periastron. Right after the periastron passage, the disc becomes unstable and all three parameters show large variability. They recover a more steady trend afterwards, with the EW rising towards previous values and both the peak separation and ratio decreasing towards values similar to those before periastron passage. The high degree of variability after the periastron passage may be directly linked to the instabilities created by tidal interactions with the neutron star, as in previous epochs the reported variability is smoother and takes place over longer time scales \citep[see][]{coe19}.

\begin{figure}
    \centering
    \includegraphics[width=0.98\linewidth]{newplot_fig2.pdf}

    \caption{Evolution of the H\,$\alpha$ parameters from the FIES spectra of MT91 213. Equivalent width measurements from \citet{coe19} are shown in red (without errors) for comparison;  the V/R ratio and peak separation are excluded because of the large errors. The lower panel shows the radius of the H\,$\alpha$ emitting region of the disc.}

    \label{fig:opt2}
\end{figure}

In order to look deeper into the detailed H\,$\alpha$  line structure, we have selected the most symmetric profiles (those at MJD$\sim$58006 and MJD$\sim$58016, when the V/R ratio is $\sim$1), and after averaging them we have subtracted that average from the rest of spectra. The results are shown in Fig.~\ref{fig:opt3}. There we can see the excess in emission moving from the right (red side) towards the left (blue side). We also see some residuals at the line wings which evolve in the opposite direction. These residuals at the wings are a consequence of the H\,$\alpha$ line asymmetry.  This asymmetry is expected for density waves perturbing the disc \citep{hummel97} and are dependent on the inclination of the disc with respect to the line of sight. The asymmetric profile in H\,$\alpha$, according to \citet{hummel97}, would correspond to a disc inclination angle of between 25 and 50 degrees.

 The peak of the excess in emission responsible of the V/R variability (Fig.~\ref{fig:opt3})
moves from a redder ($t_{\rm per} \sim -109.9$\,d) to a bluer ($t_{\rm per} \sim 49.8$\,d)  position by a distance on the order of $\sim$170\,km\,s$^{-1}$. The peak separation shown in Fig.~\ref{fig:opt2}, with an average of $\sim$290\,km\,s$^{-1}$, is also influenced by the emission excess in the line wings. The bluest peak of this wing excess at  $t_{\rm per} \sim -109.9$\,d differs in position with respect to the reddest one at $t_{\rm per} \sim 49.8$\,d on the order of $\sim$560\,km\,s$^{-1}$. This distance is in agreement with what is expected from the model of \cite{hummel97}.

The lower panel on Fig. \ref{fig:opt2} shows the evolution of the circumstellar disc radius. In order to estimate the disc radius, first  we have estimated the projected rotational velocity of MT91 213 from the peak separations  (R-V) seen in Table \ref{tab:opt1} by using the relationship
\begin{equation}
    \Delta {\rm peak} \sim (1.2\pm0.6)v_{\rm rot}\sin i
\end{equation}
which is valid for H\,$\alpha$ EWs lower than 15 \AA  \citep{hanuschik89}. We obtain a projected rotational velocity of $250\pm20$\,km\,s$^{-1}$. With this projected rotational velocity, and using the relationship \citep[see, e.g., ][]{reig16}
\begin{equation}
    \frac{R_{\rm disc}}{R_{*}}=\left(\frac{2v_{\rm rot}\sin i}{\Delta {\rm peak}}\right)^{1/j}
\end{equation}
we have calculated $R_{\rm disc}/R_{*}$. The $j$ in the exponent is expected to be $\sim$0.5 for a Keplerian disc \citep{reig16}. By fitting
\begin{equation}
    \log\left(\frac{\Delta {\rm peak}}{v_{\rm rot}\sin i}\right)=-\left(\frac{j}{2}\right)\log(-{\rm EW}_{{\rm H}\alpha})+b
\end{equation}
\citep[see][]{reig16} to the measurements from all our spectra we obtained $j\sim0.53$.

\begin{figure}
    \centering
    \includegraphics[width=0.7\linewidth]{halpha_residuals.pdf}
    \caption{Difference between all spectra in Fig. \ref{fig:opt2} and the average of the two most symmetric ones, i.e., those for which V/R ratio is $\sim$1. We see the emission excess on the wings of the line due to line asymmetry, initially on the blue side but decreasing in intensity as the V/R ration increases. This  excess appears on the red side when V/R $>$ 1 and increases in intensity afterwards. The line wing at the side of the dominant peak falls more abruptly to the continuum than the wing at the opposite side. The excess due to zones of enhanced density propagating on the disc (the cause of the V/R variability), seen in the central zone of these profiles, moves from red to blue.}
    \label{fig:opt3}
\end{figure}

\section{Results and discussion}
\subsection{Optical evidence of the Be-star disc evolution.}

The optical behaviour of PSR~J2032+4127\xspace was previously discussed by e.g.\ \citet{coe19, roucoescorial19, kolka17}.  However the majority of these observations occurred before periastron and the cadence of observations after periastron was much less. The NOT observations presented in the paper, complemented by the previous observations, show the behaviour of the disc until $\sim50$\,d after periastron.

The observations of the H\,$\alpha$ line in PSR~J2032+4127\xspace show a clear variability of the Be star disc, both in the change in equivalent width, and the V/R profile.  The equivalent width well away from periastron is $|W_\lambda|<9$\,\AA{} \citep{coe19} but becomes stronger $\sim181$\,d before periastron ($|W_\lambda|\sim15$\,\AA{}). The EW then decreases towards periastron reaching a minimum ( $|W_\lambda|\approx 6.2$\,\AA{}) a few days after periastron, while the V/R profile shows a corresponding shift to a stronger blue component and an increase in the peak separation (Fig.\ref{fig:opt1}).

The behaviour observed immediately around and after periastron is easily explained by the introduction of tidal interaction with the pulsar \citep[see the SPH modelling in ][]{coe19}.  However, the behaviour of the disc before and leading up to periastron is more challenging.

Be stars are known to show intrinsic variability of the disc structure \citep[see e.g.][and references therein]{rivinius13}, and a number of the observed changes in the disc, particularly seen far from periastron, are due to the intrinsic variability of the Be star and not the interaction with the pulsar. However, the clear variation of the EW towards periastron, with the line strength decreasing towards, and increasing after,  periastron is very suggestive that this can be attributed to the interaction in the binary system.
 It should be noted that \citet{kolka17} suggested that the behaviour of the disc around periastron was due to intrinsic variation of the star and that size of the disc remained stable as they did not measure a shift in the position of the peaks of the H\,alpha line. However, the longer period and higher resolution observations presented here and in \citet{coe19} do find a shift.

While the optical emission occurs close to the Be star (see Fig.~\ref{fig:opt2})
the disc can be much larger. For example, \citet{klement17} suggested truncation radii of $\sim100$\,$R_*$, for some Be stars, which they attributed to undetected binary companions. In the viscous decretion disc model the density of Be disc decrease with radial distance $\rho \propto r^{-n}$, and this rate is lower of Be stars in binaries due to the accumulation of material within the truncation radius, resulting in denser discs \citep[e.g.][]{zamanov01, okazaki02, panoglou16}.
The highly eccentric nature of this binary may mean that as the pulsar approaches the star truncation of the disc slows the rate at which material can flow out of the decretion disc,  causing an accumulation in material close to the star, increasing the EW. This may explain the rise in equivalent width from $|W_\lambda|<9$\,\AA{} to $|W_\lambda|\sim15$\,\AA{} between the observations before $t_{\rm per}-393$\,d and the next after $\sim t_{\rm per} - 181$\,d shown in \citet{coe19} (where $t_{\rm per}$ is the time of periastron).   There is also a clear change in the line profile with red peak significantly increasing \citep[see fig.~5 in][]{coe19}. The gravity of the pulsar could further be causing a preferential direction for the disc outflow. However, it should be noted that at these times the binary separation is still large and underlying intrinsic variability of the Be star be driving this increase \citep{kolka17}.

The observations after $\sim t_{\rm per} -181$\,d \citep[in ][and this paper; see Fig.~\ref{fig:opt2}]{coe19} show that the equivalent width peaks at $\sim t_{\rm per}-161$\,d and then steadily decreases towards periastron. The NOT observations (starting from $\sim t_{\rm per}-110$\,d) also show a general increase in the peak separation. Since Be stars are believed to be Keplerian \citep[e.g.][]{rivinius13} the peak separation traces the
dominant or average H\,$\alpha$ emission region, and the change suggests the emission region is moving closer to the Be star.
This could be occurring because as the truncation of the disc increases, the emitting region becomes smaller, decreasing the EW and moving the average emission region slightly closer to star. The disc truncation could be induced by tidal effects, but additionally the pulsar wind may be blowing away regions of the disc. This  behaviour is very different to the case of PSR~B1259-63\xspace\ where the equivalent width continues to grow past periastron.  However, the typical equivalent width of the H\,$\alpha$ line observed from PSR~B1259-63\xspace\ is much higher ($|W_\lambda|\sim 50$\,\AA{}) which suggests a much denser disc, than in the case of PSR~J2032+4127\xspace.

The influence of the pulsar is also seen in the change in the V/R profile.  While the double peaked line was symmetric ($V/R \approx 1$) far from periastron \citep[ $t_{\rm per}-600$ to $t_{\rm per}-400$\,d;][]{coe19}, after $\sim t_{\rm per}-182$\,d  the line is asymmetric and varying from redder to bluer.
The variation in V/R profile is normally attributed to density waves in the decretion disc, which in this case can be induced by the tidal interaction as is seen in SPH modelling of Be binary system \citep{okazaki02,panoglou16,coe19}.
The variation in the V/R ratio changes relatively smoothly as the pulsar approaches periastron.
However, immediately after periastron (within a few ten of days) the variation in the V/R profile and peak separation changes much more rapidly (Fig.~\ref{fig:opt2}). The peak separation reaches a maximum of 343\,km\,s$^{-1}$ before decreasing by $\sim 40$\,km\,s$^{-1}$  in $\sim3$\,d, before increase by  $\sim 40$\,km\,s$^{-1}$  within $\sim2$\,d, before decreasing again.  At the same time the V/R profile first becomes slightly redder before becoming bluer again. Because the system is highly eccentric, the binary separation at periastron is $\sim1$\,au ($\sim 28\,R_\star$), and the pulsar will introduce a strong turbulence to the disc as well as an asymmetry to the disc structure.  As the pulsar passes periastron more turbulent structures will be introduced into the disc and material can be pulled in the direction of the pulsar, then continuing to move towards us, resulting in a stronger blue component. The disc will become less symmetric and change more rapidly, causing the faster change in the V/R ratio and peak separation. This basic structure is seen in the  SPH models presented in \citet{coe19} where the disc becomes asymmetric and material is carried away from the disc.

During the post-periastron period the equivalent width starts to increase and we interpret this as the disc starting to increase in size as the binary separation increases.

\subsection{High Energy Emission}

\begin{figure*}
\includegraphics[width=0.48\linewidth]{psrj2032_4127_lc4_1.pdf}
\includegraphics[width=0.48\linewidth]{x_optics_time_200.pdf}
\caption{  \textit{Swift}/XRT\xspace 0.3-10~keV lightcurve of PSR~J2032+4127\xspace (red squares) and the corresponding slope (green circles). Cyan points and arrows demonstrate index ($3-70$~keV) and periods of the {\it NuSTAR} observations.  Black symbols in the right panel illustrate the equivalent width of the H\,$\alpha$ line reported in this paper (filled symbols) and~\citet{coe19} (empty symbols). Vertical dashed line denotes the period of the peak of H$\alpha$ equivalent width. Horizontal  dashed line corresponds to the value of the X-ray slope equal to 1.5.}
\label{fig:xrt_lc_index}
\end{figure*}
While the optical emission detected from PSR~J2032+4127\xspace is mainly coming from the Be star and its disc, the observed X-ray emission is usually attributed to the synchrotron emission of the relativistic electrons originating from the
pulsar wind. The first X-ray detection of this system was in 2002 by
\textit{Chandra}\xspace \citep{Camilo09,ho17}, which reported the detection of a new, very faint X-ray source at the position of  PSR~J2032+4127\xspace. Subsequent observations with
\textit{Chandra}\xspace and \textit{Swift}/XRT\xspace demonstrated a steady flux rise as the pulsar approached periastron.
The dependencies of the X-ray flux and slope on time are summarized in Fig.~\ref{fig:xrt_lc_index}.
The flux demonstrates a complicate behaviour with a sudden narrow dip close to periastron. The slope of the X-ray band spectrum hardens as the pulsar approaches the Be star, reaching a value of $\Gamma\sim1.5$ and remains constant around the periastron passage, see also \citet{Pal19} for the discussion of the spectral slope behaviour around the periastron.
Note that no significant variation of the hydrogen column density was detected and for the presented analysis it was fixed to its mean value over the orbit,  $N_H=0.884\cdot 10^{22}$~cm$^{-2}$. The correctness of the X-ray slopes measured by \textit{Swift}/XRT\xspace  (which can be biased due to a correlation with $N_H$) is supported by \textit{NuSTAR}\xspace measurements. These measurements performed at $>3$~keV energies are minimally affected by the absorption and are in a good agreement with the \textit{Swift}/XRT\xspace results.

Contrary to the X-ray band, the flux and the spectral slope of PSR~J2032+4127\xspace remained stable in the GeV band for the whole observational period including the periastron passage, see  \citet{li18} and Fig.~\ref{fig:lat_lc}.

Previously, the time evolution of PSR~J2032+4127\xspace was modelled by~\citet{li18} (radio, X-ray and GeV bands) and~\citet{coe19}(optics and X-ray).
\citet{li18} suggested that the strong X-ray dip close to periastron is explained by an increase of the magnetization parameter of the star--pulsar colliding winds shock accompanied by flux suppression due to Doppler boosting effect. The
post-periastron rise could be a consequence of the Be stellar disc passage by the pulsar. The absence of variability in the GeV emission was explained by the strong dominance of the pulsar magnetospheric emission over the expected orbital-modulated Inverse Compton (IC) emission. The model was able to predict the overall shape of the orbital X-ray lightcurve, but was not able to reproduce the details of the double-peak flux structure around periastron. The origin of the hardening of the X-ray spectrum, as the pulsar approaches periastron, also does not appear in the model in a natural way and was attributed by the authors to a possible increase of the hydrogen column density.\footnote{Please note, that only the hardness ratio was evaluated by~\citet{li18} .}

\citet{coe19} reported on optical and X-ray flux measurements of PSR~J2032+4127\xspace,  accompanied by  SPH modelling of the Be star/pulsar interaction. In their model the authors explicitly assumed that the disc of the Be star is inclined to the orbital plane. The modelling, however, failed to describe the details of the observed X-ray lightcurve of the system, generally predicting a maximum of the flux at periastron and
does not consider the variability of the X-ray spectrum.

Additionally, \citet{ng19} recently presented radio to X-ray observations of PSR~J2032+4127\xspace. The authors suggested a potential spectral break at $\sim 5$~keV energies which was attributed to the modification of the spectrum of accelerated electrons by synchrotron losses without detailed modelling.

Below we propose a simple model for the observed emission from PSR~J2032+4127\xspace  which allows  the observed multi-wavelength evolution
of this system to be  qualitatively explain. Within this model, similar to~\citet{coe19}, we suggest that the disc of the Be star is inclined to the orbital plane.

We would like to note that the inclination of the disc to the orbital plane was also proposed for other gamma-ray binary systems, e.g. PSR~B1259-63\xspace~\citep{melatos95,chernyakova06} and HESS J0632+057~\citep{we_hessj}. These systems demonstrate similar lightcurve with two peaks in X-ray band separated by a dip at periastron and  are characterised by a long (longer than a year) orbital period.
Such similarities allow us to speculate, that the ``inclined disc'' geometry can be typical for long-period Be-star hosting gamma-ray binaries. Inclined disc models have also been proposed for Be/X-ray binary systems \citep[see e.g.][and references therein]{brown19}. The reason for this could be that the systems are either too young or that the compact object spends too little time near the optical star to allow tidal forces to align the orbit of a compact source.

\begin{figure}
\includegraphics[width=\linewidth]{lat_lc}
\caption{ \textit{Fermi}/LAT\xspace lightcurve of PSR~J2032+4127\xspace (1-10 GeV) with a 100~days bins. The black dashed line and shaded region illustrate the best-fit of the data with a constant and the corresponding $1\sigma$ uncertainty area. }
\label{fig:lat_lc}
\end{figure}
\begin{figure*}
\includegraphics[width=0.48\linewidth]{timescales}
\includegraphics[width=0.48\linewidth]{electrons_spectrum}
\caption{Left: Synchrotron and IC cooling times along with characteristic acceleration timescale for electrons. Right: Spectra of electrons produced by the ``cooling'' and ``acceleration'' scenarios. }
\label{fig:tcool}
\end{figure*}
\subsubsection{Spectrum formation}
\label{sec:spectrum_formation}
Similar to previous works (see e.g. \cite{takata17})  we propose that the X-ray and TeV emission observed from PSR~J2032+4127\xspace  originates from synchrotron and inverse Compton (IC)
processes, respectively. The X-ray photon slope of $\Gamma\sim1.5$ allows the slope of corresponding electron spectrum to be estimated as $\Gamma_e\sim2$. At the same time the level of unpulsed radio emission reported by~\citet{ng19} does not allow a simple continuation of $\Gamma\sim 1.5$ from radio up to X-ray energies and thus suggests the presence of a low-energy feature (break or a cut-off) in the electron spectrum.
In what follows below we discuss two possible mechanisms for the formation of such a spectrum, namely the cooling and acceleration scenarios.

\noindent\textit{\textbf{Cooling scenario:}} close to mono-energetic electrons ($E_e\sim 20$~TeV) are continuously injecting by the pulsar wind at the pulsar-stellar wind interaction region. Continuous synchrotron and IC losses lead to the formation of the modified electrons spectrum and subsequently the observed X-ray and TeV emission.

\noindent\textit{\textbf{Acceleration scenario:}} similarly to the \emph{cooling scenario} mono-energetic electrons are injected, but the energy is much lower
($E_e\sim 0.1$~TeV). The injected electrons accelerate at the pulsar-stellar winds interaction shock on a characteristic timescale
\begin{equation}
t_{\rm acc} \approx 0.1\left(E_e/1\,\mbox{TeV}\right)\eta (B_0/1\,\mbox{G})^{-1}\quad\mbox{s}
\label{eq:t_acc}
\end{equation}
where $B_0$ is a magnetic field at the shock and $\eta\geq 1$ is the acceleration efficiency~\citep[see e.g.][for the details]{khangulian08}.

For typical magnetic field values considered for gamma-ray binaries, this timescale is much shorter than the synchrotron and IC loss timescales for the electrons with energies $\lesssim 100$~TeV. The acceleration of the electrons can lead to the fast formation of a
power-law (with a cut-off) electron spectrum
with a slope of $\Gamma_e \sim -2$ (typical for Fermi acceleration) and a cut-off at $\sim 30$~TeV energies. The accelerated particles escape from the system on a timescale of $t_{esc}\gtrsim d_*/c\sim 500$~s.
This approach is similar to the one used by \cite{takata17}.

The left panel of Fig.~\ref{fig:tcool} illustrates the cooling times for electrons due to synchrotron and IC (using the approximation of~\citealt{khangulian14}) emission for the parameters typical for Be-star gamma-ray binary systems (magnetic field $B_0=0.2$~G; distance from the star to the emission region $d_{*}=0.7$~au). The red dot-dashed line shows the acceleration time (Eq.~\ref{eq:t_acc}) and horizontal black dot-dashed line shows the  escape time from the system (selected to be of the order of $10^3$~s), while the dash blue and solid green lines show the synchrotron and IC cooling times, respectively.  For these representative parameters it can be seen that the synchrotron and IC cooling timescales are longer than the escaping time at low energy ($E_e<5\times10^{12}$eV) and do not modify the electron's spectrum. However, at higher energies the synchrotron cooling time  is short enough to substantially modify the injected spectrum (see the right panel of Fig. \ref{fig:tcool}).

The electron spectrum for both the cooling and acceleration scenarios is determined by numerically calculating the synchrotron and IC losses of a continuously injected spectrum of electrons, until a steady solution is obtained.  The electrons are assumed to be injected with a mono-energetic (cooling scenario) or a power-law with an exponential cutoff (acceleration scenario) spectra.  The resulting electron spectra are shown in the right panel of  Fig.~\ref{fig:tcool}.

\subsubsection{Spectral modelling}
As the pulsar start to approach to periastron ($t_{\rm per}-600$\,d) the interaction of the pulsar wind with the wind of the Be star shifts the emission region towards the pulsar. The subsequent increase of the magnetic field in the emission region naturally explains the observed rise of the X-ray flux.

The optical observations clearly demonstrates the influence
of the pulsar on the state of the Be-star disc. The interaction of the pulsar wind with the disc of the Be star leads to the
rise of the X-ray emission. At $t_{\rm per}-160$\,d the equivalent width of the H\,$\alpha$ line reaches its maximum and at around the same time the X-ray photon index becomes equal to $\Gamma=1.5$.
Such a value can be expected in either the case of acceleration in a strong shock (acceleration scenario) \citep[e.g.][]{1994ApJS...90..561J,2013APh....43...56B} or effective cooling (cooling scenario) \citep[e.g.][]{1970RvMP...42..237B}. This slope value remains almost constant up to hundred days after periastron.

The rapid strong decrease of the flux close to periastron ($t_{\rm per}-20$ to $t_{\rm per}+10$\, d)
corresponds to the pulsar entering a sparser regions due to the inclined Be-star disc. This consequently shifts the wind-wind interaction region further away from the pulsar and decreases the magnetic field in the emission region.
The shift of the emission region closer to the star can also explain the evolution of the observed TeV emission. This emission is produced by the IC mechanism from the same population of electrons which form the X-ray component of the observed spectrum. Contrary to X-ray light curve there is no dip at  periastron, but it rather demonstrates an increase in flux. This is in line with the proposed model, as the shift of the emission region towards the Be star implies an increase in the density of the soft photons and consequently an increased level of TeV emission reported by~\citet{psrj_tev}. The drop of the TeV flux immediately after the periastron is roughly coincident with second X-ray maximum and can be attributed to the attenuation of Be star's photons by dense regions of the disk.

\cite{takata17} studied details of the X-ray and TeV light curves in the scenario similar to the acceleration one. This work was done before the actual periastron passage took place and lacked knowledge of system parameters. This model didn't consider the possibility of the disc inclination and attributed two peaks in the X-ray light curve to the interplay between the orbital dependence of magnetisation parameter and Doppler boosting. Subsequent observations demonstrated that the model should be adjusted to explain the observed shape and positions of X-ray peaks.

The GeV emission observed by \textit{Fermi}/LAT\xspace is stable along the whole orbit (see Fig.~\ref{fig:lat_lc}) and in our model this is produced by the pulsed magnetospheric emission from the pulsar. The quality of the data doesn't allow to observe the variability of the GeV emission predicted by \cite{takata17}.

The X-ray to TeV SED of the system is shown in Fig.~\ref{fig:spectrum} along with the results of spectral modelling of the system. Green symbols illustrate the available data close to periastron: VLA (triangles; \citet{ng19}), \textit{NuSTAR}\xspace(squares), \textit{Fermi}/LAT\xspace(circles), VERITAS and MAGIC(semi-transparent areas; \citet{psrj_tev}). The green semi-transparent diamond points show the\textit{NuSTAR}\xspace spectrum taken at $\sim -400$~days before the periastron passage. The solid and dashed curves present the results of broad-band spectral modelling of the system for the ``cooling'' and ``acceleration'' scenarios.

The synchrotron and IC emission was calculated with the \texttt{naima v.0.8.3} package \citep{naima}, which uses the analytic approximations for the IC and synchrotron emission developed by~\citet{aharonian81,aharonian10,khangulian14}.
The solid red line in Fig.~\ref{fig:spectrum} shows the result for the ``acceleration'' scenario and corresponds to an emitting region located at a mean distance of  $d=0.7$~au from the star, a magnetic field strength of $B_0=0.2$~G and an escape time from the system of $t_{esc}=10^3$~s.
The spectral modelling of the  ``cooling'' scenario (blue dashed curves) for the same location of the emitting region requires a slightly higher magnetic field ($B_0=1$~G), and does not suggest the escape of electrons from the system. For both scenarios we assume the star to have a luminosity of  $L_*=6\cdot 10^{37}$~erg/s and a temperature $T_*=3\cdot 10^4$~K. The presented spectra directly correspond to the electron spectra shown in right panel of Fig.~\ref{fig:tcool}.

\begin{figure}
\includegraphics[width=\linewidth]{xray_tev_spectrum}
\caption{The radio to TeV spectrum of PSR~J2032+4127\xspace. The green  symbols illustrate the spectrum of the source close to periastron: VLA(triangles) \textit{Fermi}/LAT\xspace (circles), \textit{NuSTAR}\xspace(squares), VERITAS and MAGIC(semi-transparent regions). The green diamonds  show the \textit{NuSTAR}\xspace spectrum of PSR~J2032+4127\xspace measured at $\sim -400$~days before to periastron. The curves show the  results of the broad-band spectral modelling of the system for the ``cooling'' (blue dashed) and acceleration (red solid) scenarios; see text for details. The radio and TeV data are from~\citet{ng19, psrj_tev}. }
\label{fig:spectrum}
\end{figure}

\iffalse \subsection{Optics to X-ray connection}
\todo[inline]{0. Strong B/R separation indicates close to the disc plane line of sight?}
\todo[inline]{1. Evolution of B and R wavelengths (not just peaks separation): "larger" disc seems to rotate faster and smaller -- slower in Coe's paper; is it due to changes in density profile due to tidal disc-pulsar interaction?; Can we have the same points for our observations?}
\todo[inline]{2. B/R ratio changes before the periastron passage -- pulsar first builds-up "red" part of the disc (red increases, log(B/R) decreases ; $-EW$ increases; tidal interactions ) and then cuts it (red decreases, log(B/R) increases; $-EW$ decreases ); can we trace directly B and R evolution (not just the ratio?)}
\todo[inline]{3. $-EW$ behaviour in comparison to X-rays. Max $-EW$ roughly corresponds to the beginning of $-1.5$ X-ray slope. Max $-EW$ -- the moment of first effective electrons' acceleration. Before -- acceleration is not effective, slope is soft. After -- pulsar destroying the disc (cutting away outer part), but acceleration is effective. X-rays increase since density of the inner part of the disc increases (up to exit of the pulsar from the disc)}
\todo[inline]{4. Gradual increase of the disc size ($-EW$) as pulsar passed through the disc 2nd time -- tidal interactions. Gradual decay of the disc when pulsar is far away.}
\todo[inline]{5. re-plot all figs 2 as $t-t_{per}$}
\todo[inline]{6. discuss pulsed radio?}
\todo[inline]{7. Discuss B-R peaks separation, mid Fig.2?}

The observations of the H\,$\alpha$ line show a clear variability as the Be star disc, both in the change in equivalent width, and the V/R profile.  The equivalent width away from periastron $|W_\lambda|<10$\,\AA{} \citep{coe19} but is stronger $\sim100$\,d before periastron ($|W_\lambda|\sim15$\,\AA{}). The EW then decreases towards periastron reaching a minimum ( $|W_\lambda|\approx 6.2$\,\AA{}) a few days after periastron, while the V/R profile shows a corresponding shift to a stronger blue to red component and an increase in the peak separation (Fig.\ref{fig:opt1}).

The behaviour of the disc around periastron can be explained by the variations introduced by tidal interactions and the pulsar wind. As the pulsar starts to approach periastron the EW increases.  This could be due to either the disc extending in the direction of the pulsar or because the size of the disc is limited and there is an increase in the density of the disc near the region that produces H\,$\alpha$ emission.\todo{references to support this idea?}

As the pulsar gets closer to the optical companion, tidal forces can introduce an asymmetry to the disc. Assuming the disc is rotating in the same direction as the orbital motion, and based on the orientation of the binary \citep{ho17} this could preferential results in more material in the direction of the pulsar, which will be moving away from us, resulting in V/R$<1$, observed a few hundreds of days before periastron.

However, this would imply that the disc extends to very large distances from the Be star. The peak in the EW occurs $\sim160$ days before periastron \citep{coe19}, around the approximately the same time the X-ray spectrum approaches and index of $\Gamma \approx 1.5$. However, at this time the binary separation is still $\approx 7$\,au $\approx 150 R_{*}$ (assuming $M_*=10M_\odot$ and $R_*=10 R_\odot$).  This is much further than the distances implied by the H\,$\alpha$ line which implies a disc size of $\sim 14 R_*$ \citep{coe19}.  Using the relation of \citet{hanuschik89}
\begin{equation}
    \log (R_{\rm disc}/R_*) = 0.4 + 0.64 \log(-{\rm EW}),
\end{equation}
would imply the disc size decrease down to $\approx8R_*$ ($\sim0.4$\,au) at periastron).

As the pulsar moves towards and past periastron, the variation in the disc changes, with the V/R ratio shifting towards a stronger red component as well as showing more rapid variability in the disc V/R profile. The pulsar passing around periastron will introduce a strong turbulence to the disc as well as an asymmetry to the structure.  As the pulsar passes periastron more turbulent structures will be introduces into the disc and material can be pulled in the direction of the pulsar, then continuing to move towards us, resulting in a stronger blue component. This basic structure is seen in the  SPH models presented in \citet{coe19} where the disc becomes asymmetric and material is carried away from the disc.

\fi

\subsection{Comparison to other ``inclined disc'' systems}

While the  ``inclined disc'' geometry proposed for PSR~J2032+4127\xspace would suggest that it should be very similar to other gamma-ray binaries (e.g. PSR~B1259-63\xspace or HESS~J0632+057\xspace), the system's behaviour during the periastron passage does not exactly resembles the behaviour of these other systems.
While, similar to PSR~B1259-63\xspace and HESS~J0632+057\xspace, PSR~J2032+4127\xspace demonstrates a double-peaked X-ray lightcurve with a deep minimum at periastron, contrary to these systems there is no hints of orbital variations of the hydrogen column density.
The orbital X-ray spectral variability (which shows significant spectral hardening close to periastron) is also different from PSR~B1259-63\xspace \citep[softening of the spectrum close to periastron,][] {psrb2014} and HESS~J0632+057\xspace \citep[constant slope,][]{we_hessj}.

In the optical band, the differences in the behaviour of the H\,$\alpha$ emission line,  between PSR~J2032+4127\xspace and PSR~B1259-63\xspace systems are clearly seen.  In contrast to what is observed in PSR B1259-63 \citep[see][]{psrb2014} where the EW (which is linked to the disc size) increases as the neutron star approaches periastron, our data set, and that of \cite{coe19},
shows the EW reaches a maximum about 180\,d  before periastron.
But afterwards, in response to the proximity of the compact companion the disc size decreases again to levels similar to those shown in \citet{coe19} at epochs earlier than MJD$\sim$57700 (a few hundreds of days before periastron). After the periastron passage, all the H\,$\alpha$ parameters show fluctuations, and after $\sim$50 days they slowly and smoothly recover to reach values similar to those before periastron. We interpret this as disruptions caused by the tidal interaction with the compact object. Another difference is that while,  for PSR~B1259-63\xspace,  the increase in the equivalent width is steeper than the decrease, in PSR~J2032+4127\xspace we find the opposite behaviour.  Both PSR~B1259-63\xspace and PSR~J2032+4127\xspace  show evidence of a tilted disc with respect to the orbital plane. The main difference between them is that the former one has a bigger, denser,  and very stable disc  ~\citep{psrb2014} while disc in the latter is smaller and unstable \citep{coe19}. Since in both cases the pulsar crosses the disc near periastron the most dramatic effects seen in PSR~J2032+4127\xspace can, therefore, be interpreted as a consequence of the properties of its circumstellar disc.
  A comparison between how the pulsar disrupts a lower density and a higher density circumstellar disc can be seen in the SPH  modelling shown in fig.~1 \& 2 of \citet{takata12}. There the authors compare, for PSR~B1259-63\xspace, the pulsar approaching the star/circumstellar disc for a base density of $\rho_0 = 10^{-11}$ and $10^{-9}$\,g\,cm$^{-3}$.

The maxima of the (absolute value) equivalent width of the H\,$\alpha$ line are offset from the peaks of X-ray lightcurve (see Fig.~\ref{fig:xrt_lc_index}, right panel). Assuming that the X-ray flux maxima correspond to the moments of the plane of the disc-crossing, we conclude that the disc has a maximal size \citep[(see e.g.][]{grundstrom06}) significantly before and after disc crossing events. This can be understood, if a few competing processes take place in this system, e.g. star-pulsar tidal interactions (increasing disc size and build-up rate, as the pulsar approaches the periastron) and perturbations of the disc by the pulsar wind (continuous destroyment of the disc which leads to gradual decreasing of its size, e.g. sharp cutting the disc at distances higher than pulsar-star separation, see e.g.~\citep{monageng17,coe19}). Note that in \citet{takata17} it was demonstrated that if the base density is less than
$\rho_0 < 10^{-10}$ g/cm$^3$, the pulsar wind can strip off an outer part of the Be disk, truncating it at a radius smaller than the pulsar orbit,
and only the post-periastron X-ray flare may be related to disc crossing \citep{li18}.

The magnetic field in the emitting region typically considered for PSR~B1259-63\xspace is about $\sim 1$~G~\citep[see e.g.][]{psrb2014} which is comparable to values found here within the cooling scenario and somewhat higher than what is required for the acceleration scenario ($\sim 0.2$~G). In terms of the energetics the spin-down luminosity of PSR~B1259-63\xspace exceeds that of PSR~J2032+4127\xspace by a factor of 5 \citep{romoli17, psrj_tev}, while the spatial scales of both systems at periastron are comparable ($\sim 1$~au).
The higher magnetic field in PSR~B1259-63\xspace allows fast and more efficient cooling of the pulsar wind's electrons via synchrotron losses at timescales shorter or comparable to PSR~J2032+4127\xspace. Within the cooling scenario this should lead to a similar formation of a low-energy tail in the spectrum of electrons. The characteristic tail's slope of $\Gamma_e = -2$ should result in an X-rays slope of $\Gamma \sim -1.5$ during the periods of disc crossing. Contrary, significant spectral softening (up to photon X-ray slope $\sim -2$) was observed during these periods~\citep{psrb2014}. Such a discrepancy is challenging  to explain within the ``cooling scenario'', however it could be understood within ``acceleration scenaio''.

Fig.~\ref{fig:tcool} (right panel) illustrates how different values of the magnetic field in the emitting region modify the final electron spectrum, for an initially injected cut-off powerlaw (with the slope of $-2$) electron spectrum in the "acceleration scenario". Namely, the increased value of the magnetic field leads to a significant softening of the spectrum at energies comparable to the injection energy ($\sim 0.1$~TeV). The electron spectrum is modified in a similar way for a constant magnetic field but for longer electron escape times.

Within the ``acceleration scenario'' significant softening of the electrons' spectrum (and consequent softening of X-rays) during the disc crossing in PSR~B1259-63\xspace can be understood if the emitting region approaches the pulsar (magnetic field in the region increases) and/or escape time from the system significantly increase when the pulsar enters dense disc regions.
The weaker H\,$\alpha$ emission line observed in PSR~J2032+4127\xspace suggests that the disc is smaller than in in PSR~B1259-63\xspace.  This means that
during the whole periastron passage, PSR~J2032+4127\xspace remains in a lower-density regions (than in PSR~B1259-63\xspace) which results in shorter escape times
and the magnetic field in the emitting region remains relatively low. This results in a hard X-ray slope of PSR~J2032+4127\xspace system during the whole periastron passage.

\section{Conclusions}
In this paper we analyse the results of multi-wavelength observation of PSR~J2032+4127\xspace as it is approaching and passing by its periastron in 2017. The observations of the H\,$\alpha$
line  show a clear variability of the Be star disc, both in the change in equivalent width, the line separation and the V/R profile. X-ray emission from the system is also highly variable, increasing as the pulsar approaches periastron, but with a sharp minimum around the periastron itself.
A clear link between the X-ray emission and the state of the Be star disc is demonstrated by the fact  the X-ray spectral index changes at the same  moment as the H\,$\alpha$ equivalent width peaks.

The assumption that the disc of the Be star is inclined to the orbital plane allows the observed high energy variability  to be explained in a natural way.  In the proposed model  X-ray and TeV emission observed from PSR~J2032+4127\xspace  originate  from  synchrotron  and  inverse Compton  processes,  respectively. The observed spectrum from the source can be understood within the ``cooling'' or the ``acceleration'' scenario which relies on cooling/acceleration of monoenergetic electrons of pulsar wind, see Sec.~\ref{sec:spectrum_formation} for the details. While both scenarios are able to satisfactory describe the SED of PSR~J2032+4127\xspace system, we argue that ``acceleration scenario'' seems to be preferable for other gamma-ray binaries, e.g. PSR~B1259-63\xspace and thus is natural for PSR~J2032+4127\xspace as well.

\section*{Acknowledgements}
The authors acknowledge support by the state of Baden-W\"urttemberg through bwHPC.
This work was supported by DFG through the grant MA 7807/2-1, partially supported by the Spanish Government under grant PGC2018-093741-B-C21 (MICIU/AEI/FEDER, UE), and the Russian Foundation for Basic Research project 17-52-80139 BRICS-a (SST).
This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester. We acknowledge the use of public data from the Swift data archive and thanks the entire Swift team for accepting and planning Target-of-Opportunity requests.
We also acknowledge funding to support our NOT observations from the Finnish Centre for Astronomy with ESO (FINCA), University of Turku, Finland (Academy of Finland grant nr 306531). The authors wish to acknowledge the DJEI/DES/SFI/HEA Irish Centre for High-End Computing (ICHEC) for the provision of computational facilities and support. We would also like to acknowledge networking support by the COST Actions CA16214 and CA16104.

\bibliographystyle{mn2e}
\input{journals.tex}

redpajama_set_name: RedPajamaArXiv


text:
Regular readers will remember that we featured five-year-old James, who has vocal cord palsy, earlier this year. His condition means that he can only speak with a very quiet voice, due to a paralysed vocal cord. Unfortunately, when there is any background noise it is extremely difficult to hear him, particularly at school and when out and about in his wheelchair and the car. Obviously this is quite a big problem for one so young.
By David Martin
James' mum got in touch with Remap to see if their clever engineers could come up with a solution and before long Niall McCarroll, a volunteer from Remap Berkshire had paid them a visit. Remap is a charity that helps disabled people of all ages to live more independent lives by designing and making customised equipment free of charge.
Niall could immediately see that James needed some kind of amplifier for his voice and this was confirmed by Lizzie Nash, the speech therapist supporting him. She explained that adults with the condition could be supplied with a personal amplifier but that these were not available for small children.
Niall went away to design and build a special microphone, pre-amplifier and speaker that James could wear on a belt. This new gadget was then tested and found to be a great success. James could now communicate without straining his weak vocal cords. A few months after receiving the gadget, his mum says: "We are still getting on really well with the voice amplifier. By far the biggest impact has been at school. He is talking with his peers now and is happy to speak up in class. He can be heard in the classroom and so can contribute independently to discussions and whole group work, rather than having to rely on the voice of his teaching assistant. It has also helped his confidence. He can be more independent as we now feel more confident that we will hear him if he needs help – rather than having to keep him in sight at all times."
She went on to say: "Amazingly the speech therapists have actually noticed an improvement in his voice quality since he's been wearing it consistently! Probably because he's no longer straining and trying to make himself heard. It's beyond what we'd hoped for!"
"He is talking with his peers now and is happy to speak up in class."
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This attractive traditionally styled wicker type commode includes a vinyl waterproof cushion, a conventional style lavatory seat and pot with a lid. Seat width 50cm, height 49cm. Weight carrying capacity 115kg (18 stone).


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During the initial months of a prospective epidemiologic investigation of coronary heart disease in middle-aged Puerto Rican men, it was readily apparent that subjects with low serum cholesterol values were being encountered with unusual frequency. Of the first 2,000 individuals examined, 49% had cholesterol values below 200 mg/100 ml, and 12% had values less than 160 mg/100 ml (1).
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Scotsman Alexander McDougall (1845-1924) was a ship captain on the Great Lakes when he patented the idea of a "whaleback" ship in the early 1880s. With low, rounded hulls, decks and deckhouses, his invention minimized water and wind resistance. Between 1887 and 1898, 44 whalebacks were produced: 23 were barges and 21 were steamships, including one passenger vessel.
Frank Rockefeller was the 36th example of the type, built in 1896 at a cost of $181,573.38 at McDougall's American Steel Barge Company in Superior, WI. One of the larger examples of the type, Rockefeller measured 380 feet in length, drew 26 feet of water depth and had a single propeller.
Although it belonged to several different owners over its 73-year working life, the Rockefeller spent most of its early life transporting iron ore from mines in Lake Superior to steel mills along the shores of Lake Erie. In 1927, new owners put it in service as a sand dredge that hauled landfill sand for the 1933 Chicago World's Fair. From 1936-1942 the old ship saw service as a car carrier for another set of owners. In 1942 the ship wrecked in Lake Michigan, but wartime demand for shipping gave the old ship repairs, a new name (Meteor) and a new life as a tanker transporting petroleum products for more than 25 years. In 1969 Meteor ran aground off the Michigan coast, Instead of repairing the old ship, the owners sold it for a museum ship at Superior, WI. In poor condition today, Meteor is the last surviving example of McDougal's whaleback or "pig boat".


I thought I have all in life and think I am happy. I can afford everything, and have them in a minute. I don't care how many people hated me because of how I deal with them. For me, money is good enough for them to shut up.
I got all these things because of my hard work, and I always believe in me. I still believe everything I can do, and no one will surpass me. I just want to have a comfortable life, to do everything I like and make things possible. But I always feel a lack in myself. I know I am living my dreams, but it is always not enough. Maybe because it is hard for me to forgive, and still have not moved on from a painful past. I don't have any friends, distance from my family and hated any commitments. I have changed because I feel like people being so abusive and took me for granted.
I got a hatred from my family, who abandon me and leave me. And now they will suddenly show up and ask for help. I don't have any mercy for them even though my mom battling cancer. She told me she has no one with her anymore; he lived in a partner leave her because she is useless now and added a headache to him. She has asked for forgiveness many times and sorry for her actions. But the damage has been done, and no matter how I tried myself to forgive her, I can't give her what she wants. Nobody had loved me when I asked for love before. I beg her not to go away because I am afraid of the dark and being alone. But she left me crying and joined her partner. I am so sad, spent many days alone and cried because of fear but no one hears me. I go on a day without food and strive hard to earn money. She does not show up on those days of my life.
My girlfriend also did the same thing, Kimmy is the only woman I trusted before. I met her at our school where I was granted a scholarship. Both of us are a scholar and have the same dreams in life. Just like me, she has also hatred for her parents and wants to get away from them. We promise to be together to each other through thick and thin. Right after our graduation, we part ways to work. Later on, she broke up with me because she is not happy with me anymore.


Overkill Strike is a classic first person shooter game with multiplayer component! You can find a bunch of FPS games on both Android and iOS app store but almost all of them shares the same concept and gameplay. Some, however, managed to give a unique approach to the game and provide their game an all new appeal. So where exactly Overkill Strike weighs in? I decided to download Overkill Strike to provide you an in-depth review and to see what exactly this game has to offer.
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Overkill Strike features basic controls. Prior to the battle, the players will pick the location they prefer. After selecting, the game prompts you to the battlefield. You can freely navigate around the map using the virtual joystick while you can shoot by tapping the bullet icon. The player can also activate the Auto Fire option or choose to shoot manually. Aiming is done by moving the crosshair around the screen. If the Auto Fire is on, the gun shoots automatically to wherever the crosshair is pointing. You can also jump and throw flash bomb or grenade.
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Aside from different location, the game also has different weapons that players can unlock. On top of your default weapons, the game also allows you to either buy or rent extra guns. If your money is not enough to buy guns permanently, you can rent them for certain number of days instead. You can rent guns through virtual cash or diamonds (premium currency). Each weapon can be rented for 1 or 3 days. You can also customize the skins and apply miscellaneous accessories. You can access all these items through the Shop.
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Overall, Overkill Strike might fall into a basic FPS category. There's nothing grand about the game but still decent and enjoyable enough to play with. The graphics are smooth with some minor glitches and bugs but still tolerable. If there are things we want to see in its future development, it's probably new campaigns. A Career Mode or Special Multiplayer Events can be an interesting addition to the game. Nevertheless, if you love FPS, this game is fair enough to meet your expectation.