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Home FEATURED POSTS Indie Band Non Duo Shares Joy and Love in their Music
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Indie Band Non Duo Shares Joy and Love in their Music
by adminupdated on July 15, 2016 July 25, 2016
Paul: "It's tough. There are lots of sharks."
There's a sort of predatory wing of the industry. It's like in nature when there are lots of little fish gathering for something (indie artists in L.A.) bigger fish (fake radio promotors, "producers") will show up and have an easy meal.
Marina: "I see it a bit different. When we first get a spark to create, we do it for the pure joy of it, and then we want the whole world to share in that joy. Our job is to be the vehicles for what wants to be created and the Universe's job is to wink back at us. Sometimes that wink comes in a form of a business contract and lots of views and money, but more often it comes in a form of creating itself." @nonduo1
http://www.blogtalkradio.com/avaliveradio/2016/07/21/episode-343-ava-live-radio-behind-the-music-with-jacqueline-jax
GETTING TO KNOW NON DUO
by Jacqueline Jax host of A.V.A Live Radio
Non Duo (Paul McCarty and Marina Gutman)
Based in Los Angeles
There's a sort of predatory wing of the industry. It's like in nature when there are lots of little fish gathering for something (indie artists in L.A.) bigger fish (fake radio promoters, "producers") will show up and have an easy meal.
Marina: "I see it a bit different. When we first get a spark to create, we do it for the pure joy of it, and then we want the whole world to share in that joy. Our job is to be the vehicles for what wants to be created and the Universe's job is to wink back at us. Sometimes that wink comes in a form of a business contract and lots of views and money, but more often it comes in a form of creating itself."
Marina: "Failure is just another way of asking: Do you really want to do this? If the answer is yes, then it's no longer a failure. More specifically, I've gotten rejected after every initial pursuit of a passion and it's my steady resolve that has prevailed in the end. And now people say, "It's easy for you, you've been a creative person all your life," not knowing what goes on behind the stage."
We never really considered doing anything less
than a full album while planning to record as Non Duo, though we plan to pre-release the "Free" video with our recorded version of the song because there's such a strong buzz on it. But we write pretty prolifically together so cutting down to an album was hard enough. I've never felt compelled to put out an EP, and singles (I've been told by promoters) are just harder to promote. A full album just feels like you're making a real statement to the world.
Social Media allows indie artists to get their music out there quickly and efficiently,
and it lets us interact with our people on a daily basis. It allows for excitement-building even before the album is released. We put out a teaser with stills from our upcoming videos and music as a way to get people talking and excited about what's to come. We've got interested parties waiting for the album, people telling us they can't wait to buy it. We are also planning to use social media to release each of our videos individually, spanning a week or so, in order to build even more suspense right before we release the album. We will do the same when we put out our events for the album release concerts.
Paul: "I'm sure John Lennon would be fun and very enlightening to talk to."
Marina: "The Buddha. Who else do you need?"
A handful of people get excited by something
that no one could've predicted or controlled and then someone else calls it "trendy" and "current". No true artist does his/her art to try and be trendy. They just do it and if it's recognized and becomes popular, then that is by definition trendy. For instance, after we translated the Russian song, people were asking us to do more. We tried to translate another cool song, but all the ones we attempted so far felt forced and unorganic. So we decided not to force it unless one pops up spontaneously like "Free" had done.
Our Yoga teacher's favorite phrase
with which to end every pose: "Ok. That's good enough."
Paul: "I've been playing music since I was a kid."
My mom and dad were both musicians. For decades I tried to make a living at film scoring. It was when I relaxed on the making-a-living part that I started enjoying it more. I formed a band (Wicked Saints) and we recorded two albums and two singles together."
Marina: "I've been singing since I was a kid, but didn't start pursuing it seriously until I got jealous hearing another woman singing one of the songs that I wrote with Paul. Then it was on. Inspiration comes in many forms. For many years it's been fiction writing and then it branched out into songwriting and eventually singing."
It's the only cover song on our upcoming album.
It's "Raft" by Yury Loza and it's the first thing that we collaborated on. Marina thought that I should cover it with Wicked Saints, so we worked together on the translation from the Russian original, then sent it to the songwriter for approval. To our surprise he actually worked some on it with us and then approved it when he was happy with it. Turns out it's a big deal because it's never been sung in English before and it was a huge song in the '80s in the USSR. Everyone knows it.
A man is so disillusioned with society/life/the world that he gets on a raft and sets off for who-knows-where and never returns.
Support Artist: https://itunes.apple.com/us/album/dark-single/id1053950801
Paul recorded a live video of the song with Wicked Saints
and once Russia found out it existed, it went totally viral. Marina and I recorded our version and are hoping for similar success of it as Non Duo.
Well, our name Non Duo comes from the term non-dual,
which means not two, but one, as in underneath the seeming difference between us, we're all the same. Most of our songs to varying degrees touch on that theme such as Dark, Shadows and Lights, Small Things, Turn Around, and (believe it or not) there's also a song called Not Two. And we'd like to think that even our translation could help bridge the gap between two worlds.
There are many places to play and hear live music. Although there is a smorgasbord of places to go, it's a challenge for the indie artist because there are many of us here in LA and it's a buyer's market.
We opt for no-cover intimate listening-room venues.
Some of the places where we play are Muse on 8th, State Social House on Sunset Strip, Matt Denny's Ale House in Arcadia, Brennan's Pub in Marina Del Rey, Viva Cantina in Burbank, and many others.
We both enjoy Yoga.
Recently we discovered a passion for making music videos—both the making of and the process of editing.
Website: https://www.non-duo.com
Youtube: https://www.youtube.com/watch?v=2tMJ7ycSvNo
Facebook: https://www.facebook.com/nonduo1/?fref=ts
Twtter: https://twitter.com/nonduo1
Soundcloud: https://soundcloud.com/non-duo
Tags: music marketingmusic newsNon DuoThe Music Business
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NEWS POINT HILL
Family mourns Point Hill singer slain in Spanish Town
A family is still trying to come to grips with the gun murder of an aspiring artiste, who was best known in Point Hill district, St. Catherine.
The deceased is 34-year-old Clary Peters, otherwise called 'Ryan'. In entertainment circles, he used the name 'Sahsick'. He also was a shop operator.
Relatives told The Beacon that Peters is originally from a rural community in St. Ann, but he left that parish in his early teens to join his maternal family in St. Catherine.
Peters lived in Point Hill for a number of years before he recently relocated to join his second son's mother in Spanish Town, St. Catherine.
The Jamaica Constabulary Force (JCF) said Peters also lived at Old Market Street in Spanish Town, but was killed at the intersection of Hanover Street and William Street.
The shooting took place on the morning of Sunday, February 14 – Valentine's Day. That's also 10 days before the victim's birthday.
The JCF said: "Reports from the Spanish Town Police are that, about 9:30AM, Peters was at his shop when he was approached by a man on foot. The man, who was armed with a handgun, reportedly opened gunfire at him, hitting his upper body. He was taken to the hospital by citizens where he was pronounced dead. Investigations are ongoing."
In the meantime, a close cousin of the deceased who spoke on condition of anonymity, said he and the late Peters spent many childhood years together.
In a recent conversation that unfolded between the two, Peters reportedly said he was planning to travel to St. Ann.
The cousin further told The Beacon: "Ryan was jovial – jovial, jovial, jovial. I can't say that too much. He wasn't a warmonger. If you listen his music, it is something about girls. Him nuh do gun songs; him humble."
Police yet to identify charred human remains found in Point Hill
Linstead | Alleged gunman killed during home invasion

redpajama_set_name: RedPajamaCommonCrawl


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Essential workers who have coronavirus get help with benefits (video)
Taken from NJSpotlight.com
By Michael Hill
It's a major shift in New Jersey's workers' compensation law. During the health emergency, essential workers no longer have to prove they contracted the coronavirus on the job to qualify for workers' compensation benefits. Gov. Phil Murphy signed it into law Monday, retroactive to March 9.
"They're required to go to work. They go there, they get sick and then, under the old worker's compensation system, they would have to keep proving, it would be very difficult, they would have to prove that they got the COVID at work," Sen. Linda Greenstein (D-Middlesex) said.
The new law shifts the burden of proof from the employee to the employer. One nurse from Virtua Memorial Hospital says the law will be a game changer.
"I'm thinking of one member in particular who had a prolonged hospital stay for a documented at-work exposure and she's still having problems getting her workman's comp," said Sheryl Mount, president of Health Professionals and Allied Employees Local 5105. "The news of this passing to her was a godsend."
"Workers who sacrificed their health to take care of these desperately sick patients should never have to take on their employer," said Debbie White, the president of Health Professionals and Allied Employees.
The new law also applies to gas station attendants and automotive and convenience store workers.
"It's unfair, and mostly it's unreasonable, to pass a law with a presumption, an automatic presumption, that an employee contracted the COVID-19 virus while at work," said Sal Risalvato, executive director of the New Jersey Gasoline, Convenience, Automotive Association.
A maskless mob that greeted social media influencer Nelk Boys in Seaside Heights led to disorderly conduct citations.
"It was irresponsible from top to bottom in every respect," Gov. Phil Murphy said at Wednesday's coronavirus briefing.
Read more and watch the video here.


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Deutsche accused of spying on its staff
Updated: 05:01 EST, 22 July 2009
Germany's biggest bank was last night facing a possible criminal investigation amid claims that it spied on troublesome staff and investors.
Surveillance: Deutsche is accused of snooping on staff
Deutsche Bank is reported to have sacked two workers over allegations that it bugged two board members and one renegade shareholder.
State prosecutors are looking into the accusations with a view to mounting a criminal case against Deutsche.
The surveillance allegedly took place as far back as 2001, although the most lurid claims dates back to 2006, when the bank is accused of spying on activist shareholder Michael Bohndorf.
Bohndorf, a lawyer who lives in Ibiza, told Germany's Spiegel magazine that a 'honeytrap' involving a 'delicious' Brazilian woman may have been set for him.
Deutsche has acknowledged that it spied on Gerald Herrmann, a former member of its non-executive supervisory board, after it suspected him of leaking information to a journalist for news agency Reuters.


Professional headshots are a great investment for your career. Make sure you get the most out of your investment by considering these suggested tips to help you prepare for your session.
Get plenty of rest the night before your shoot. Being well rested will not only make you feel refreshed, you'll look refreshed, too!
Eat a healthy breakfast and/or lunch prior to your session. Try to stay away from greasy, fatty foods. This will make sure you feel great and have sufficient energy levels throughout your shoot.
Consider this: Bring a power snack to give you an energy boost if you need one (nuts, granola, energy bar, whiskey, etc).
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Consider this: Bring a bottle of water with you so you can hydrate as needed, especially during summer months.
If you are planning to get your hair trimmed, restyled or planning any drastic changes to your appearance, we recommend that you do this at least (1) week before your shoot. New styles and fresh haircuts will need a little time to fill in before you are camera ready.
What to bring: Comb, hairbrush, hairspray or any other hair care products you typically use. You may need to touchup during your shoot.
Doing your own makeup? Keep your makeup and style simple. Try not to get too adventurous with your look unless that is your usual style. A little makeup can go a long way in a portrait. Remember, we are going for a professional and natural look.
What to bring: Extra makeup in case you need any touch ups during your shoot.
Hiring our makeup artist? Follow your normal makeup and grooming routine the day of your shoot. This will give our stylist a starting point for your typical look, then they will make you camera ready from there.
Its best to shave or do any beard trimming the morning of your shoot. Take your time when shaving to limit any razor burn or cuts. If you plan on getting a haircut, we recommend that you do this at least (1) week before your shoot. Fresh haircuts will need a little time to fill in before you are camera ready.
Clothing with solid, neutral colors are the best choice for a professional headshot. The main focus will be on your eyes and face, so make sure that your clothing choices don't draw attention away from this. Also, keep in mind clothing choices that complement your skin tones.
Layering clothing is a great way to achieve multiple looks without the need to change while on location. Scarves, sweaters, suits or other jackets, and even glasses.
Consider this: Bring a couple of your best shirt, tie or jacket options and we can look over it together to decide what will work best.
Stay away from busy patterns, large logos and overly bright clothing. Bright color choices can reflect unwanted color onto your face. Reconsider accessories or jewelry that is distracting in shape or color. Remember, the focus is on you so let's keep it simple.
Wear a comfortable pair of walking shoes. Usually we will need to walk around our location to find great backdrops and lighting. You can always change your shoes for full body shots once we reach the shoot location.
The weather in Portland, Oregon can be unpredictable, so bring proper outdoor attire for the weather (jacket, umbrella, etc.).
Take some extra time in front of the mirror to practice the look you want. Move your face in different positions and note the subtle changes of angles and light. Slightly turn your face side to side, chin up/down, wide eyes/focused eyes, push your nose forward/back, laugh/smile/smirk/stoic. This exercise will not only give you a visual of what the camera sees, but it will also help you better understand the direction we will give during your shoot.
Wear what makes you feel confident and comfortable. You know what you look good in, so wear it! If you are confident in how you look, that confidence will come through in your headshots.
Confidence and preparation are the key to capturing great headshots. Come prepared to have some fun and we'll get some great headshots with the time we have!


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Freedom Bowl: Prairie's Jake Clark offers special dedications
Date: Monday, July 15, 2019
Football player honors a great family friend, and other families in crisis
VANCOUVER — He showed up to practice, proudly wearing his Prairie helmet, ready to represent the Falcons at the Freedom Bowl Classic.
A closer look at the helmet revealed a date.
"April 5, 2019."
Jake Clark and his family lost a dear friend that day.
Jake Clark of Prairie shows off a special date on his helmet prior to Saturday's Freedom Bowl Classic. He dedicated the game to a family friend, who passed away on that day.
That friend, Bill Joyce, was friends with Jake's dad, Rob Clark, for 50 years.
Since kindergarten.
A half-century of friendship.
Bill was not family by blood, but he was family.
And this is a football family, too.
Jake Clark is planning to continue his football career at Pacific University in Forest Grove.
Bill and Rob had a plan, too. They were going to tailgate at Pacific, then watch Jake take the field.
"I put the date on there because it means something for my family," Jake Clark said.
He dedicated the game to Bill, to honor not just Bill but also Jake's dad. He wanted to let everyone know just how special of a bond those two had, and how that great relationship inspired their children.
The gesture was special to Rob.
"Jake came to me and said, 'Dad, I have one high school game left. I'd like to dedicate it to Bill.' He understands the meaning of family and good friends. That's the simplest way to say it. He knows what it means to be surrounded by good people."
So on Saturday night at McKenzie Stadium, Jake Clark played his final high school game, helping the West beat the East all-stars 6-0 in the 2019 Freedom Bowl Classic. Clark, a linebacker, had six tackles in the shutout.
There is more to this dedication, though. You see, Jake announced to his family what he was going to do before Freedom Bowl week. During the week, though, he was among the players who visited Shriners Hospitals for Children in Portland. This game, after all, is a charity event put on by local Shriners.
Clark decided to do a double-dedication.
"It's not just his dedication," Jake said of Bill Joyce. "It's also for all the families going through hard times."
He saw some patients at the hospital, he got a tour detailing the facility, and he learned about the hardships so many families must endure when their children are sick or injured.
There are those who cannot play football, now or never, or any other sport. He wanted to play for them, too.
"This is for those who are no longer with us or who can't do it," Clark said.
When he was younger, Jake and his dad used to come to the Freedom Bowl Classic, as fans.
"I just remember thinking, 'One day, I want to be here.' To actually be here, it's a dream come true," Jake said.
Overall MVP:
Carter Morse of Hudson's Bay forced two fumbles and seemed to be in just about every play on defense. And on offense, he scored the only touchdown with a diving catch in the fourth quarter. For his efforts, he was named the game's overall MVP.
Commitment: Over the years, the Freedom Bowl has extended its boundaries, allowing for more schools to participant. That makes for a long drive for some of the players. One, Cole Dorman, played 8-man football at Naselle.
He made it to practice all week — that's a four-hour round-trip — and it paid off for him. A quarterback, he earned the West's offensive MVP award for his touchdown pass.
The other MVPs: Ridgefield's Makani Schultz was the defensive MVP for the West squad. On the East team, Jacob Leckie of Evergreen was the defensive MVP and Evergreen running back Trent Hemann was named the top player on offense.
Salute: Here is a shout-out to all who played this year. It is not easy giving up a week in the summer, especially for those players coming from the coast. It is also difficult for coaches and players to find the right mix for quality execution. There is a limited practice schedule. Still, the game has a great cause. And those who play, coach, and officiate, you are appreciated — Paul Valencia
Tags:Brush PrairieClark CountyLatestVancouver


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Cameron Diaz and Drew Barrymore have been long-time pals ever since they starred in Charlie's Angels together, and it appears their bond is stronger than ever.
In a recent interview with presenter Andy Cohen on his SiriusXM radio show, Cameron revealed that she's got her friend's back, in light of the recent news that Drew is getting divorced.
"Everybody pulls the wagons around, you know, our friends, whoever needs us at whatever point in time, even if it's like something that the public doesn't know about. Internally we're all going like, 'Okay, who needs us now?'"
Last week, Drew revealed that she is set to divorce her husband of almost four years Will Kopelman, with whom she has two daughters Olive, 3, and Frankie, 23 months.
The actress also posted up a picture supporting Cameron's new tome, The Longevity Book.
In the same interview, Cameron revealed details about her wedding to musician Benji Madden, who she married last year.
"We got married in our living room in front of our friends,' the actress told radio host Andy Cohen of the intimate ceremony. '[We] had a little party in our backyard on the tennis court and yeah. Otherwise it would have been something else."


text:
Deborah Gates
dgates@delmarvanow.com
UMES is considering its stand on an honorary degree awarded to actor and comedian Bill Cosby.
It is not alone. Scores of colleges and universities that have held Cosby in high esteem have been grappling with how to respond to allegations of sexual assault by 60 or more women against the 78-year-old entertainer and role model over generations.
Among those that awarded Cosby honorary degrees over the years — by published accounts, about a dozen or more, including Goucher in Maryland — have rescinded the honor since allegations began flaring a year or more ago.
That's an option at UMES, said President Juliette Bell in a written comment, expressing disappointment. The university names Patrick Liverpool, provost and vice president for academic affairs, at the helm of an evaluation of options, with leadership making a final decision.
"We are dismayed at the recent charges and will continue to assess our options, one of which is to rescind the degree," Bell said.
A final decision on the issue would be made by the University System of Maryland Board of Regents, the president said. It is undecided whether UMES would submit a recommendation in time to be on the board's Feb. 12 agenda, if at all. "No determination has been made," the university commented in a statement. "The matter is still under review."
Mike Lurie, University System of Maryland spokesman, said he was unaware of any universities in the system "forwarding such a request to the USM regarding rescission of an honorary degree to Bill Cosby at this point in time." He also said universities would initiate a request to the board for action, the same protocol for recommending an honorary degree.
For UMES, the issue has raised the question of the type of degree that was bestowed upon the iconic star of "The Cosby Show." Cosby was the university's 1998 spring commencement speaker, and the event was held at the Wicomico Youth & Civic Center because of an expectant huge crowd.
"The May 17, 1998, graduation program on file does not list the type of honorary degree he received," the university said.
An article about the commencement in the May 20, 1998, edition of the Somerset Herald said that then-UMES President Dolores Spikes awarded the celebrity an honorary university degree, and offered that he had "given us the benefit of his heart and soul today."
According to a university system guideline, honorary degrees are awarded to "individuals who have made exceptional contributions in intellectual, scholarly, or creative areas; or b. individuals who have risen to a position of eminence in their chosen field or who have acquired a national or international reputation in a selected field or endeavor; or c. individuals who have compiled a record of distinguished public service."
Students contacted at random favored Cosby keeping the honorary degree, saying it represents his talent and public service, not his misjudgements. Some cited his role as a model to African-Americans in general, and his contributions to historically black colleges in particular.
"Growing up I admired Bill Cosby and I still admire Bill Cosby," said Jamar Armstrong, a freshman student from Princess Anne. "What he did was wrong, but everybody deserves a second chance. I feel sorry for Bill Cosby. UMES nor any other college should take anything away from Bill Cosby."


KANEOHE, OAHU (HawaiiNewsNow) - Honolulu firefighters rescued three hikers from the Koolau Summit Trail.
Firefighters first responded on Thursday around 7:20 p.m. to reports that the hikers, all in their late 20s, were lost and couldn't find their way down the trail. However, they were uninjured and in a safe location.
After arriving on scene, HFD airlifted one of the three hikers, but weren't able to get to the other two because of weather conditions. They were instructed to shelter in place until first light the next day.
HFD resumed rescue operations around 6:40 a.m. Friday, with both hikers being airlifted to a nearby landing zone.


text:
Conquering the Woman é um filme mudo norte-americano de 1922, do gênero drama, dirigido por King Vidor. Uma cópia do filme existe na Koninklijk Belgisch Filmarchief, na Bélgica.

Elenco
Florence Vidor ... Judith Stafford
Bert Sprotte ... Tobias Stafford
Mathilde Brundage ... Tia Sophia
David Butler ... Larry Saunders
Roscoe Karns ... Shorty Thompson
Peter Burke ... Conde Henri
Harry Todd ... Sandy MacTavish

Filmes mudos
Filmes dos Estados Unidos de 1922
Filmes de drama dos Estados Unidos
Filmes de romance dos Estados Unidos
Filmes em língua inglesa
Filmes em preto e branco

redpajama_set_name: RedPajamaWikipedia


text:
North Dakota Rules of Court
RULE 1.1 SCOPE RULE 2.2 FACSIMILE TRANSMISSION [REPEALED] RULE 3.1 PLEADINGS RULE 3.2 MOTIONS RULE 3.3 CHANGE OF JUDGE FOR POSTJUDGMENT MOTION OR PROCEEDING RULE 3.4. PRIVACY PROTECTION FOR FILINGS MADE WITH THE COURT RULE 3.5 ELECTRONIC FILING IN DISTRICT COURTS RULE 4.1 APPOINTMENT OF GUARDIAN AD LITEM [REPEALED EFFECTIVE MARCH 1, 2000] RULE 4.2 NOTICE TO INTERESTED PARTIES [REPEALED] RULE 8.3.1 CASE MANAGEMENT (DETERMINATION OF PARENTAL RIGHTS OR CHANGE OF RESIDE APPENDIX A TO RULE 8.9. CODE OF MEDIATION ETHICS RULE 5.1. INTERSTATE DEPOSITIONS AND DISCOVERY RULE 5.2 EXTRAORDINARY WRITS RULE 5.3 RECEIVERS RULE 5.4 PETITION FOR RESTORATION OF FIREARMS RIGHTS RULE 6.1 CONTINUANCES RULE 6.2 OPENING STATEMENTS RULE 6.3 PARTIES' ORDER OF PROCEEDING RULE 6.4 EXHIBITS RULE 6.5 [REPEALED] RULE 6.6 BENCH WARRANT RULE 6.7 JUROR NOTE TAKING RULE 6.8 QUESTIONING BY JURY RULE 6.9 ASSISTING JURORS AT IMPASSE RULE 6.10 COURTROOM OATHS RULE 6.11 PREDELIBERATION DISCUSSION BY JURORS RULE 7.1 JUDGMENTS, ORDERS AND DECREES RULE 7.2 RECOGNITION OF TRIBAL COURT ORDERS AND JUDGMENTS RULE 8.1 FAMILY MEDIATION PROGRAM RULE 8.2 INTERIM ORDERS IN DOMESTIC RELATIONS CASES RULE 8.3 CASE MANAGEMENT (DIVORCE CASES) RULE 8.4 SUMMONS IN ACTION FOR DIVORCE, SEPARATION OR TO DETERMINE PARENTAL RIGH RULE 8.5 DOMESTIC RELATIONS SUMMARY PROCEEDING RULE 8.6 PARENTING INVESTIGATORS RULE 8.7 GUARDIAN AD LITEM RULE 8.8 ALTERNATIVE DISPUTE RESOLUTION RULE 8.9 ROSTER OF ALTERNATIVE DISPUTE RESOLUTION NEUTRALS RULE 8.10. COLLABORATIVE LAW RULE 8.11. Parenting Coordinators RULE 8.12 NOTICE IN ACTION TO TERMINATE PARENTAL RIGHTS RULE 8.13 IN CHAMBERS INTERVIEW OF CHILD IN DOMESTIC RELATIONS CASE RULE 8.14. TERMINATION OF CHILD SUPPORT ORDER RULE 9.1 ADMINISTRATIVE APPEALS RULE 10.1 CONDUCT IN COURT RULE 10.2 SMALL CLAIMS COURT RULE 11.1 NONRESIDENT ATTORNEYS NOT LICENSED IN NORTH DAKOTA [SUPERSEDED] RULE 11.2 WITHDRAWAL OF ATTORNEYS RULE 11.3 STIPULATIONS RULE 11.4 BONDS IN NON-CRIMINAL MATTERS RULE 11.5 SANCTIONS RULE 11.6 MEDIUM-NEUTRAL CASE CITATIONS RULE 11.7 TITLE AND CITATION APPENDIX A. SUMMONS IN ACTION FOR DIVORCE OR SEPARATION APPENDIX B. FINANCIAL STATEMENT AND AFFIDAVIT APPENDIX C. RULE 8.3 INFORMATIONAL STATEMENT APPENDIX D. PRETRIAL CONFERENCE STATEMENT RULE 8.3 APPENDIX E. RULE 8.3 CONFIDENTIAL PROPERTY AND DEBT LISTING APPENDIX F. RULE 8.8 ALTERNATIVE DISPUTE RESOLUTION STATEMENT APPENDIX G. CODE OF CONDUCT FOR PARENTING INVESTIGATORS Appendix I. N.D.R.Ct. 8.1 Family Mediation Program Forms Appendix J. N.D.R.Ct. 3.5 Electronic Filing Forms APPENDIX K. RULE 3.5 ELECTRONIC FILING REQUIREMENTS APPENDIX L. RULE 8.3.1 INFORMATIONAL STATEMENT APPENDIX M. RULE 8.3.1 SCHEDULING ORDER
RULE 8.7 GUARDIAN AD LITEM
(a) Qualification. To qualify as a guardian ad litem under N.D.C.C. § 14-09-06.4, a person must be an attorney licensed in the state of North Dakota.
(b) Training Requirements. To be eligible for appointment as a guardian ad litem, an attorney must have completed 18 hours of guardian ad litem training. To remain eligible to be appointed as guardian ad litem, an individual shall complete an additional 18 hours of guardian ad litem-related training every 3 years.
(c) Criteria for Appointment. A guardian ad litem must be appointed if the court finds an appointment is necessary to protect the best interests of the child involved. In determining whether to appoint a guardian ad litem, the court shall consider among other factors:
(1) whether there is an allegation of sexual abuse;
(2) whether there is an allegation of domestic violence resulting in serious bodily injury or involving the use of a dangerous weapon;
(3) whether there is an allegation of a pattern of domestic violence occurring within a reasonable time proximate to the proceeding resulting in a reasonable fear for the safety of a party or the minor child;
(4) whether the child has special needs;
(5) whether the child has, at any time, been placed in foster care, or in the home of a third party;
(6) whether there is an allegation the child is in an unstable environment;
(7) whether there has been repeated post-decree litigation involving parental rights and responsibility issues;
(8) whether the interests of the child and either or both parents are in substantial conflict;
(9) whether a guardian ad litem could provide the court with significant information not otherwise available or likely to be presented by the parents; and
(10) whether there are any other areas of special concern which may impact the best interests of the child.
(d) Responsibilities of Guardian ad Litem.
(1) A guardian ad litem shall advocate the best interests of the child as to parental rights and responsibility and support. A guardian ad litem shall function independently, in the same manner as an attorney for a party to the action, and, consistent with the Rules of Professional Conduct, shall consider, but not be bound by, the wishes of the child or others as to the best interests of the child.
(2) After appointment, a guardian ad litem shall:
(A) work with a parenting investigator, if appointed, to coordinate investigation activities and avoid duplicating services;
(B) interview and observe the child to ascertain the facts relevant to parental rights and responsibilities, the child's wishes, the need for independent evaluation, and the need for and appropriateness of interim judicial relief;
(C) advise the child and the child's parents of the role and responsibilities of the guardian ad litem;
(D) interview potential witnesses, lay and expert, with relevant knowledge of the child or parties; and
(E) participate in meetings impacting the life of the child, including permanency planning meetings and other activities as may be directed by the court.
(3) A guardian ad litem may apply for a court order to protect the child, to obtain temporary relief, to determine parenting rights and responsibilities.
(4) A guardian ad litem shall participate whenever any party requests an interim court order which may affect the child.
(5) A guardian ad litem may request an independent court-ordered evaluation or study, including a parenting investigation.
(6) A guardian ad litem shall participate in all pretrial procedures and negotiations and endeavor to resolve the case without the need for a trial.
(7) A guardian ad litem shall observe all statutes, rules, and regulations concerning confidentiality. A guardian ad litem may not disclose or participate in the disclosure of information to any person who is not a party to the case, except as necessary to perform the guardian ad litem duties or as may be specifically provided by law.
(e) Court Proceedings. A guardian ad litem may present a case, cross-examine a witness, deliver a summation, prepare a memorandum of law, file a motion, and file or participate in an appeal on issues involving the best interests of the child.
Rule 8.7 was adopted, effective March 1, 2000; amended effective August 1, 2009.
The role of a guardian ad litem is to act as an attorney. A guardian ad litem is not to act as a parenting investigator by preparing a parenting investigation report or giving testimony.
SOURCES: Joint Procedure Committee Minutes of May 21-22, 2009, pages 44-45; September 24-25, 1998, pages 8-15.
Obsolete Date
08/01/2009 View
03/01/2000 08/01/2009 View


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text:
Multiple Dwellings
Section 4.07 - PHFL Section 33(1)(c)
Limited-Profit Housing Companies
(UDC subsidiary other than not-for-profit) PHFL Section 33(1)(c)
Related Statutes: None SUMMARY:Real property that (1) is owned or under the control of a limited-profit (Mitchell-Lama) housing company which is a subsidiary of the NYS Urban Development Corporation (UDC) but is not organized on a not-for-profit basis, or (2) was once owned by such a housing company and has been sold to another limited-profit housing company with the approval of the State Commissioner of Housing, and (3) is used for low-income or middle-income housing is partially exempt from taxation, but is liable for special ad valorem levies and special assessments. The amount of exemption is limited to that part of the assessed value which exceeds the value of the property at the time of acquisition by the original limited-profit housing company (subject to minimum limits on taxes payable as described under Limitations on Exemption below).
Ownership Requirements: Land and improvements (1) must be owned or under the control of a limited-profit (Mitchell-Lama) housing company which is a subsidiary of the UDC but is not organized on a not-for-profit basis or (2) must have been acquired by a limited-profit housing company from such a UDC subsidiary. To qualify as a UDC subsidiary, more than half of the voting shares of the housing company must be held or owned by the UDC or more than half of the directors, trustees, or members of the company must be UDC designees. The specific organizational requirements are as follows:
Limited-profit (Mitchell-Lama) housing company (co-op):
Law under which incorporation required: PHFL Article 2.
Restrictions on corporate purposes or activities as stated in certificate of incorporation: (1) Company must be organized to plan, acquire, construct, own, maintain, and operate housing projects subject to the supervision of the State Commissioner of Housing or other appropriate agency, (2) no director or subscriber of the company may receive, in repayment of his investment in the company's stock, any sum in excess of the par value of the stock, together with such dividends or other compensation permitted under PHFL Article 2, and (3) company's housing projects must, to the extent of at least 80%, be occupied by persons or families entitled to occupancy through ownership of shares in the company.
Limited-profit (Mitchell-Lama) housing company (other):
Restrictions on corporate purposes or activities as stated in certificate of incorporation: (1) Company must be organized to plan, acquire, construct, own, maintain, and operate housing projects subject to the approval of the State Commissioner of Housing or other appropriate agency and (2) no director or subscriber of the company may receive, in repayment of his investment in the company's stock, any sum in excess of the par value of the stock, together with such dividends or other compensation permitted under PHFL Article 2.
Property Use Requirements: Property must be used for housing for low-income or middle-income persons. For a description of the income limits for low-income persons, see Chart ID, PHFL Article 2, 31. The statute sets no limits on the income of middle-income persons.
Certification by State or Local Government: Amount of tax exemption due to rental assistance payments under U.S. Housing Act 8 must be certified annually by the State Commissioner of Housing, the NYC Department of Housing Preservation and Development, or the comptroller or other chief fiscal officer of a municipality outside New York City, as appropriate.
LOCAL OPTION: Not for the initial exemption. However, an existing exemption may be extended for an additional period following the expiration of the initial tax exemption period (see Limitations on Exemption below).
Taxes School
Taxes Special
Tax Special
1. Amount Yes* Yes* No
2. Duration Yes** Yes** No
Ex-Exemptâ â â â â â Tax-Taxableâ â â â â â NA-Not Applicable
* Amount of exemption is limited to that part of the assessed value which exceeds the value of the property at the time of acquisition by the original limited-profit housing company. In addition, taxes paid must not be less than 10% of the annual shelter rent or carrying charges of the project. ( Shelter rent" equals the total rents received from occupants of a project minus the cost of providing electricity, gas, heat, and other utilities. Total rents may or may not include rent supplements and subsidies from the federal government, the state, or a municipality on behalf of the occupants, but do not include interest reduction payments received under 201(a) of the Federal Housing and Urban Development Act of 1968. In the case of co-op projects, carrying charges, rather than shelter rents, apply.)
** Duration of exemption is limited to the period during which the mortgage loans of the original housing company, including any additional mortgage loan, if approved by the State Commissioner of Housing & Community Renewal or other supervising agency, the proceeds of which are used primarily for the residential portion of the project, are outstanding and the project continues to be operated as a limited-profit housing project. (The provision covering additional mortgage loans was enacted on June 30, 1989, became effective as of July 1, 1987, and applies to any projects whose tax exemption expired on or after July 1, 1987. Reinstatement of the exemption on affected assessment or tax rolls must be done through the correction of clerical errors or unlawful entries, whichever is appropriate, as described in RPTL Title 3, Article 5.)
After the tax exemption period has expired, each county, city, town and village in which the property is located may choose to grant an additional exemption period, of up to 50 years, or until such time as the project no longer complies with the operating requirements of the Mitchell-Lama Program, whichever is sooner.
General Municipal and School District Taxes: 100% of that part of the assessed value which exceeds the value of the property at the time of acquisition by the original limited-profit housing company (subject to minimum limits on taxes payable as described under Limitations on Exemption above).
Code Description of Alternative Codes Possible
Assessment Roll Section(s): Taxable (RPS Section 1).
NOTE: This code should not be used to identify (1) property that is owned by a UDC subsidiary organized under the NPCL and PHFL Article 2 and is exempt under RPTL §422 or (2) property that is exempt under any of the statutes listed under Similar Exemptions below.
REPORTING REQUIREMENTS (Assessor): None.
SIMILAR EXEMPTIONS: See Chart IA and Chart IB.
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Please send general questions or comments to Jerome McCall


text:
\section{Introduction}
For about 6 years, the {\small CORALIE} planet-search programme in the
southern hemisphere (Udry et al., 2000) has been ongoing on the
1.2 m Euler Swiss telescope, designed, built and operated by the
Geneva Observatory at La Silla Observatory (ESO, Chile).  During
this time, the {\small CORALIE} radial-velocity measurements have allowed
us to detect close to 40 extra-solar planets.  Interestingly,
brown-dwarfs candidates, easier to detect with high-precision Doppler
surveys, seem to be more sparse than exoplanets (Mayor et al.,
1997), especially in the 10-40\,$M_\mathsf{Jup}$ interval (Halbwachs
et al., 2000), the so called {\it brown-dwarf desert}.  Objects
in this domain are very important to understand the brown-dwarf/planet
transition.  The distinction between planets and brown dwarfs may rely
on different considerations such as mass, physics of the interior,
formation mechanism, etc.  From the ``formation'' point of view, the
brown-dwarf companions belong to the low-mass end of the secondaries
formed in binary stars while planets form in the protostellar disk.
Such distinct origins of planetary and multiple-star systems are
clearly emphasized by the two peaks in the observed distribution of
minimum masses of secondaries to solar-type stars (e.g. Udry et al., 2002).
They strongly suggest different formation and
evolution histories for the two populations: below
10\,$M_\mathsf{Jup}$ the planetary distribution increases with
decreasing mass and is thus not the tail of the stellar binary
distribution.

In this context, the 17.5\,$M_\mathsf{Jup}$ minimum mass companion
detected around {\small HD}\,202206 (Udry et al., 2002,
Paper\,I) provided an interesting massive planet or low-mass
brown-dwarf candidate.  Contrary to {\small HD}\,110833 which was
detected with a comparable $m_2\sin{i}$ companion (Mayor et al.,
1997) and then was shown to be  a stellar binary (Halbwachs
et al., 2000), the distance of {\small HD}\,202206 (46.3 pc)
prevents the {\small HIPPARCOS} astrometric data from constraining the
visual orbit.  At such a distance the expected minimum displacement on
the sky of the star due to the inner companion is only 0.26 mas,
largely insufficient for the {\small HIPPARCOS} precision.  If not due to
unfavorable orbital inclination, the observed low secondary mass sets
the companion close to the limit of the planetary and brown-dwarf
domains.

Apart from the massive planet candidate, the
radial-velocity measurements of {\small HD}\,202206 also revealed an
additional drift with a slope of $\sim$\,43\,ms$^{-1}$yr$^{-1}$
pointing towards the presence of another companion in the system
(Paper\,I).  The long-term follow-up of {\small HD}\,202206 is now
unveiling the nature of the second companion: a planet about ten times
less massive than the inner one. If we assume that the outer planet was formed
in the stellar protoplanetary disk, the inner planet likely also
formed there, and therefore is not a brown dwarf. This means that
protoplanetary disks may be much more massive than usually thought.
Inversely, if we assume that the inner body was formed as a brown dwarf, then
either the outer planet was also formed as a brown dwarf, or it was formed
in an accretion disk around the binary composed of the main star and the brown
dwarf.

Dynamically, the present system is also very interesting.  The
large mass of the inner planet provokes high perturbations in the
orbit of the outer one.  The system is thus in a very chaotic region,
but the existence of a 5/1 mean motion  resonance in this region
allows it to stabilize the orbits of the planets in this system.

The stellar properties of {\small HD}\,202206 are briefly recalled in
Sect.\,2, The radial velocities and the new detected companion are
described in Sect.\,3. The stability of the system is examined in
Sect.\,4 and the possible implications of such a system on the
planet versus brown-dwarf formation paradigm are discussed further in
Sect.\,5.

\section{HD\,202206 stellar characteristics}

The {\small HD}\,202206 star was observed by the {\small HIPPARCOS}
astrometric satellite ({\small HIP}\,104903).
A high-precision
spectroscopic study of this star was also performed by Santos et
al. (2001) in order to examine the metallicity distribution of
stars hosting planets.  Observed and inferred stellar parameters from
these different sources are summarized in Table\,\ref{T1}, taken
from Paper\,I.

The high metallicity of {\small HD}\,202206 probably accounts for its
over luminosity ($M_V=4.75$, $\sim$\,0.4\,mag brighter than the
expected value for a typical G6 dwarf of solar metallicity) as
$T_\mathsf{eff}$ is also larger than the value expected for a G6
dwarf.

\begin{table}[t!]
\caption{Observed and inferred stellar parameters for {\small HD}\,202206.
Photometric, spectral type and astrometric parameters are from
{\small HIPPARCOS} (ESA 1997). The atmospheric parameters $T_\mathsf{eff}$,
log $g$, [Fe/H] are from Santos et al. (2001). The bolometric
correction is computed from Flower (1996) using the spectroscopic
$T_\mathsf{eff}$ determination. The given age is derived from the
Geneva evolutionary models (Schaerer et al., 1993) which also
provide the mass estimate.}
\llabel{T1}
\begin{center}
\begin{tabular}{l l c} \hline \hline
{\bf Parameter}  & $ \quad \quad \quad \quad \quad \quad $
& {\bf {\small HD}\,202206}\\
\hline
Spectral Type & & G6V  \\
$ V $   &       & $ 8.08 $  \\
$ B-V $ &       & $ 0.714 $  \\
$ \pi $ & [mas] & $ 21.58 \pm 1.14 $  \\
$ M_V $ &       & $ 4.75 $  \\
$ BC $  &       & $ - 0.082 $  \\
$ L  $  & $ [L_\odot] $ & $ 1.07 $  \\
\hline
 [Fe/H] &       & $ 0.37 \pm 0.07 $  \\
$ M $   & $ [M_\odot] $ & $ 1.15 $  \\
$ T_\mathsf{eff} $ & [K] & $ 5765 \pm 40 $  \\
 log $ g $ & [cgs] & $ 4.75 \pm 0.20 $  \\
$ v \sin i $ & [km/s] & $ 2.5 $  \\
 age & [Gyr] & $ 5.6 \pm 1.2 $  \\
\hline
\end{tabular}
\end{center}
\end{table}

The dispersion of the {\small HIPPARCOS} photometric data of {\small
  HD}\,202206 ($\sigma_\mathsf{Hp}=0.013$ mag) is slightly high for the
star magnitude but some indication of stellar activity is seen in the
spectra.

The radial-velocity jitter associated with intrinsic stellar activity
of rotating solar-type stars may have induced spurious radial-velocity
noise, decreasing our ability to detect planetary low-amplitude
radial-velocity variations.  Although noticeable, the activity level
of {\small HD}\,202206 is not very large (Paper\,I, Fig.\,2). It
adds only some low-level
high-frequency spurious noise in the radial-velocity measurements,
taking into account the small projected rotational velocity of the
star and the long period of the newly detected planet.

\section{Orbital solutions for the HD\,202206 system}
\llabel{orbsolutions}

The {\small CORALIE} observations of {\small HD}\,202206 started in
August 1999.  The obvious variation of the radial velocities allowed
us to announce the detection of a low-mass companion of the star
after one orbital period.  When a second maximum of the
radial-velocity curve was reached, we noticed a slight drift of its
value.  With 95 measurements covering more than 3 orbital periods, a
simultaneous fit of a Keplerian model and a linear drift yielded a
period of 256 days, an eccentricity $e$\,=\,0.43 and a secondary
minimum mass of $17.5\,M_\mathsf{Jup}$ (Paper\,I).  The slope of the
radial-velocity drift was found to be 42.9\,$\mathrm{m
  s}^{-1}\mathrm{yr}^{-1}$, and the available measurements did not allow
us to further constrain the longer-period companion.

After $105$ {\small CORALIE} radial-velocity measurements
we are now able to describe the orbit of the third body in the system.
Surprisingly, the former observed drift was not the result of a
stellar companion, but the trace of a not very massive planet in a
$1400$ day orbit with eccentricity $e=0.27$.  Indeed, the outer
planet minimum mass of $2.44\,M_\mathsf{Jup}$ is almost ten times
less massive than the inner one.

Using the iterative Levenberg-Marquardt method (Press et al., 1992),
we first attempt to fit the complete set of radial velocities from
{\small CORALIE} with a single orbiting companion and a linear drift as we did
in Paper\,I (solution {\bf S1}).  This fit implies a companion with $P=255.9$ days,
$e=0.43$ and a minimum mass of $17.7\,M_\mathsf{Jup}$ (Table\,\ref{T2}),
similar to our previous values (Paper\,I).
However, the slope of the radial velocity drift now drops to $4.96\,\mathrm{m
s}^{-1}\mathrm{yr}^{-1}$, indicating that something changed after the
consideration of the additional data. Such is also
inadequate, as the velocity residuals exhibit $rms=23.45\,\mathrm{m s}^{-1}$,
while the measurement uncertainties are only $\sim$\,8\,$\mathrm{m s}^{-1}$. In
particular, this fit gives a reduced $\sqrt{\chi^2}=3.66$, clearly
casting doubt on the model.  Using a quadratic drift instead of a
linear one (solution {\bf S2}), we get identical values for the companion orbital
parameters (Table\,\ref{T2}), and slightly improve our fit, obtaining
$\sqrt{\chi^2}=2.52$ (Fig.\,\ref{F1}).

\begin{figure}[t!]
   \centering
    \includegraphics*[height=8.5cm,angle=270]{Figures/ fig01.ps}
  \caption{{\small CORALIE} radial velocities for {\small HD}\,202206
    with a single planet and a linear drift ({\bf S1}). We see that
    many points lie outside the fitted curve and the value of the reduced
    $\sqrt{\chi^2} = 3.66 $ is unacceptable.  \llabel{F1} }
\end{figure}

\begin{table}[h]
\caption{Orbital parameters of a single companion orbiting
{\small HD}\,202206 including drifts in the fit. We consider two
cases: a linear drift ({\bf S1}) and a quadratic drift ({\bf S2}).
This last model improves
the fitted solution, but is still unsatisfactory as we also add one
more degree of freedom. $ \lambda $ is the mean longitude of the date
($ \lambda = \omega + M $) and errors are given by the standard deviation $
\sigma $.}
\llabel{T2}
\begin{center}
\begin{tabular}{l l c c} \hline \hline
{\bf Param.}  & {\bf S1 \& S2} & {\bf linear (S1)} & {\bf
quadratic (S2)}   \\ \hline
rms          & [m/s]                & $ 23.45 $           & $ 15.62 $ \\
$\sqrt{\chi^2}$     &                      & $ 3.66 $           & $ 2.52 $ \\  \hline
Date         & [JD-2400000]         &   52250.00 (fixed)             &   52250.00 (fixed)   \\
$V$          & [km/s]               & $ 14.730 \pm 0.001 $ & $ 14.752 \pm 0.001 $ \\
$P$          & [days]               & $ 255.86 \pm 0.03  $ & $ 256.04 \pm 0.03 $ \\
$\lambda$    & [deg]                & $ 263.51 \pm 0.10   $ & $ 265.04 \pm 0.12 $ \\
$e$          &                      & $ 0.431 \pm 0.001 $ & $ 0.440 \pm 0.001 $ \\
$\omega$     & [deg]                & $ 157.61 \pm 0.27   $ & $ 159.75 \pm 0.28 $ \\
$K$          & [m/s]                & $ 573.26 \pm 1.17  $ & $ 566.75 \pm 1.22 $ \\
$T$          & [JD-2400000]         & $ 52174.7 \pm 0.2   $ & $ 52175.1 \pm 0.2 $ \\ \hline
$k_l \; t$   & [m/s/yr]             & $ 4.96 \pm 0.49  $ & $ 10.69 \pm 0.55 $ \\
$k_q \; t^2$ & [m/s/yr$^2$]         & $ - $               & $ -17.29 \pm 0.66 $ \\ \hline
$a_1 \sin i$ & [$10^{-3}$ AU]       & $ 12.17 $           & $ 11.98 $ \\
$f (m)$      & [$10^{-9}$ M$_\odot$]& $ 3669  $           & $ 3497  $ \\
$m_2 \sin i$ & [M$_\mathsf{Jup}$]   & $ 17.7 $           & $ 17.5 $ \\
$a$          & [AU]                 & $ 0.83 $           & $ 0.83 $ \\ \hline
\end{tabular}
\end{center}
\end{table}

\subsection{Two independent Keplerian fits}

Here we try to fit the radial velocities with two orbiting planetary
companions moving in two elliptical orbits without interaction (solution {\bf S3}).
The orbits can thus be described by two independent Keplerians as separate
two-body problems, without accounting for mutual planetary
perturbations.

\begin{figure}[t!]
    \includegraphics*[height=8.5cm,angle=270]{Figures/ fig02.ps}
  \caption{{\small CORALIE} radial velocities for {\small HD}\,202206
    with a two independent Keplerian model ({\bf S3}). The residuals
    are smaller
    than in the case obtained with only one planet (Fig.\,\ref{F1})
    and the value of the reduced $\sqrt{\chi^2}=1.53$ is also better.
  \llabel{F2}}
\end{figure}

\begin{table}[h!]
\caption{Orbital parameters of two planets orbiting {\small
    HD}\,202206 using a two independent Keplerian model ({\bf S3}).
    We neglect the gravitational
interactions between the two planets, but we obtain a better fit than
using a single planet with a drift (Table\,\ref{T2}). Errors are given
by the standard deviation $ \sigma $.}
\llabel{T3}
\begin{center}
\begin{tabular}{l l c c} \hline \hline
{\bf Param.}  & {\bf S3} & {\bf inner} & {\bf
outer}   \\ \hline
rms          & [m/s]                & \multicolumn{2}{c}{9.81}   \\
$\sqrt{\chi^2}$     &                      & \multicolumn{2}{c}{1.53}   \\ \hline
Date         & [JD-2400000]         & \multicolumn{2}{c}{52250.00 (fixed)}  \\
$V$          & [km/s]               & \multicolumn{2}{c}{$ 14.721 \pm 0.001 $}  \\
$P$          & [days]               & $ 256.20 \pm 0.03  $ & $ 1296.8 \pm 19.1 $ \\
$\lambda$    & [deg]                & $ 265.60 \pm 0.13  $ & $ 31.54 \pm 2.67 $ \\
$e$          &                      & $ 0.433 \pm 0.001 $ & $ 0.284 \pm 0.046 $ \\
$\omega$     & [deg]                & $ 161.10 \pm 0.31  $ & $ 101.83 \pm 6.60 $ \\
$K$          & [m/s]                & $ 564.83 \pm 1.45  $ & $ 42.71 \pm 2.00 $ \\
$T$          & [JD-2400000]         & $ 52175.6 \pm 0.2   $ & $ 51206.4 \pm 29.9 $ \\  \hline
$a_1 \sin i$ & [$10^{-3}$ AU]       & $ 11.99 $           & $ 4.88 $ \\
$f (m)$      & [$10^{-9}$ M$_\odot$]& $ 3502  $           & $ 9.22  $ \\
$m_2 \sin i$ & [M$_\mathsf{Jup}$]   & $ 17.5 $           & $ 2.41 $ \\
$a$          & [AU]                 & $ 0.83 $           & $ 2.44 $ \\ \hline
\end{tabular}
\end{center}
\end{table}

The two-planet Keplerian fit to the radial velocities using the
Levenberg-Marquardt method yields for the
inner planet $P$\,=\,$256.2$ days, $e$\,=\,$0.43$ and a minimum mass
of $17.5\,M_\mathsf{Jup}$, while for the new companion
$P$\,=\,$1297$~days, $e$\,=\,$0.28$ and a minimum mass of
$2.41\,M_\mathsf{Jup}$ (Table\,\ref{T3}).  The velocity residuals in
this two-planet model drops to $rms$\,=\,$9.81\,\mathrm{m s}^{-1}$ and
the reduced $\sqrt{\chi^2}$ is now $1.53$, clearly suggesting that
the two companion model represents a significant improvement, even
accounting for the introduction of four additional  free parameters.
The Levenberg-Marquardt minimization method rapidly converges into local minima
of the $ \chi^2 $. However, there is no guarantee that this minimum is global.
Thus, we also fitted our data using a genetic algorithm starting with
arbitrary sets of initial conditions. The found orbital parameters are
identical to the Levenberg-Marquardt solutions. We hence conclude
that our $ \chi^2 $ value is the best for the present data.

The necessity of the second planet is demonstrated visually when we
compare Figs.\,\ref{F1} and \ref{F2} showing {\small CORALIE} radial
velocities and the associated residuals.
In Fig.\,\ref{F3} we plotted the orbit of the second planet in the radial
velocity residuals of the inner planet.
We also show the frequency analysis of this data and a respective
periodogram of the velocity residuals. The largest frequency peak ($ \approx
0.0007 \, \mathrm{day}^{-1} $) corresponds to the period of the outer planet
and there are no aliases.
Finally, we computed false alarm probabilities for the second planet through
Monte Carlo simulations by randomly shuffling the data.
The dotted line in the power spectra of the inner planet residuals
(Fig.~\ref{F3}) shows the height of the largest aleatory peak obtained after
100,000 random simulations. The amplitude of this peak is $ 0.023 $~m/s, that
is, about one half of the amplitude of the main peak of the second planet
spectra ($ \approx 0.045 $~m/s).
This gives a false alarm probability of less than $ 10^{-5} $.

\begin{figure}[t!]
   \begin{tabular}{c}
    \includegraphics*[height=8.5cm,angle=270]{Figures/ fig03a.ps} \\
    \includegraphics*[width=8.5cm]{Figures/ fig03b.ps}
   \end{tabular}
  \caption{{\small CORALIE} residual radial velocities for
    {\small HD}\,202206 when the contributions from the inner planet
    are subtracted (top) and respective frequency analysis and periodogram. The
    data acquired before JD=2452200 showed a
    linear trend that could be provoked by a distant binary companion.
    However, the data acquired after that date clearly shows a short
    period companion.
    The dotted line in the power spectra shows the height of the largest
    aleatory peak obtained after 100,000 random Monte Carlo simulations.
    This corresponds to a false alarm probability of less than $ 10^{-5} $.
     \llabel{F3}}
\end{figure}

\subsection{Planet-planet interaction}

\llabel{planet_planet_interaction}

Due to the proximity of the two planets and to their high minimum
masses (in particular to the inner planet's huge mass), the
gravitational interactions between these two bodies will be quite
strong.
This prompt us to fit the observational data using a 3-body model (solution {\bf S4}),
similarly to what has been done for the system GJ\,876 (Laughlin and
Chambers, 2001, Laughlin et al., 2004).  Assuming co-planar
motion perpendicular to the plane of the sky, we get slightly better
results for $\sqrt{\chi^2}$ and velocity residuals (Table\,\ref{T4})
than we got for the two-Keplerian fit.  The improvement in our fit is
not significant, but there is a striking difference: the 3-body fitted
orbital parameters of the outer planet show important deviations from
the two-Keplerian case.
We then conclude that, although we still cannot detect the
planet-planet interaction in the present data, we will soon be able to
do so.  We have been following the {\small HD}\,202206 system for
about five years and we expect to see this gravitational interaction
in less than another five years. Thus, two complete orbital
revolutions of the outer planet around the star should be enough.  In
Fig.\,\ref{F4} we plot the two fitting models evolving in time and we
clearly see detectable deviations between the two cruves appearing in
a near future.

Finally,
we also fitted the data with a 3-body model where the inclination of
the orbital planes was free to vary (as well as the node of the outer
planet).  We were unable to improve our
fit, even though we have increased the number of free parameters by
three.  Therefore, the inclination of the planets remains unknown, as
do their real masses.

\begin{figure}[t]
   \begin{tabular}{c}
    \includegraphics*[height=8.5cm,angle=270]{Figures/ fig04a.ps} \\
    \includegraphics*[height=8.5cm,angle=270]{Figures/ fig04b.ps}
   \end{tabular}
  \caption{Radial velocities differences between the two independent
    Keplerian model (Table\,\ref{T3}) and the 3-body model
    (Table\,\ref{T4}).  Data coincides at JD=2452250 (Dec. 6th 2001).
    In the bottom figure we plotted the velocity residuals of the two Keplerian fit.
    Since {\small CORALIE}'s precision is about 8~m/s for this star, we expect
    to observe these differences in the coming years.  \llabel{F4}}
\end{figure}

\begin{table}
\caption{Orbital parameters of two planets orbiting {\small HD} 202206
using 3-body model ({\bf S4}). We take into account the gravitational
interactions between the two planets, but we obtain a similar fit to
the two-Keplerian model (Table\,\ref{T3}). However, the orbital
parameters of the outer planet are different.
Errors are given by the standard deviation $ \sigma $.}
\llabel{T4}
\begin{center}
\begin{tabular}{l l c c} \hline \hline
{\bf Param.}  & {\bf S4} & {\bf inner} & {\bf
outer}   \\ \hline
rms          & [m/s]                & \multicolumn{2}{c}{9.65}   \\
$\sqrt{\chi^2}$     &                      & \multicolumn{2}{c}{1.47}   \\ \hline
Date         & [JD-2400000]         & \multicolumn{2}{c}{52250.00 (fixed)}   \\
$V$          & [km/s]               & \multicolumn{2}{c}{$ 14.721 \pm 0.001 $}  \\
$P$          & [days]               & $ 255.87 \pm 0.06  $ & $ 1383.4 \pm 18.4 $ \\
$\lambda$    & [deg]                & $ 266.23 \pm 0.18  $ & $ 30.59 \pm 2.84 $ \\
$e$          &                      & $ 0.435 \pm 0.001 $ & $ 0.267 \pm 0.021 $ \\
$\omega$     & [deg]                & $ 161.18 \pm 0.30  $ & $ 78.99 \pm 6.65 $ \\
$K$          & [m/s]                & $ 564.75 \pm 1.34  $ & $ 42.01 \pm 1.50 $ \\
$i$          & [deg]                & $ 90.00 $ (fixed)   & $ 90.00 $ (fixed) \\  \hline
$a_1 \sin i$ & [$10^{-3}$ AU]       & $ 11.96 $           & $ 5.15 $ \\
$f (m)$      & [$10^{-9}$ M$_\odot$]& $ 3487  $           & $ 9.51  $ \\
$m_2 \sin i$ & [M$_\mathsf{Jup}$]   & $ 17.4 $           & $ 2.44 $ \\
$a$          & [AU]                 & $ 0.83 $           & $ 2.55 $ \\ \hline
\end{tabular}
\end{center}
\end{table}

\section{Orbital stability}
\llabel{section_orbital_stability}

In this section we briefly analyze the dynamical stability of the
orbital parameters obtained in the previous section.  A more detailed
study of the system behavior will be presented in a forthcoming paper.

\begin{figure*}[t!]
   \begin{tabular}{c c}
     two independent Keplerian model ({\bf S3}) &
     3-body dynamical model ({\bf S4}) \\
    \includegraphics*[width=8.5cm]{Figures/ fig05a.ps} &
    \includegraphics*[width=8.5cm]{Figures/ fig05b.ps} \\
    \includegraphics*[width=8.5cm]{Figures/ fig05c.ps} &
    \includegraphics*[width=8.5cm]{Figures/ fig05d.ps}
   \end{tabular}
  \caption{Dynamical evolution of the semi-major axes and eccentricity for
    two different sets of initial parameters. On the left we plotted
    the evolution for S3 initial parameters obtained with a two
    independent Keplerian model (Table\,\ref{T3}), while on the right
    we used the S4 initial parameters from the 3-body dynamical model
    (Table\,\ref{T4}). Both sets of initial parameters are unstable,
    although S4 is a little better (the outer planet
    is only lost after forty thousand years).  \llabel{F5}}
\end{figure*}

\subsection{Dynamical evolution}

In last section we saw that there were two different models to fit the
observational data: a simplified model using independent Keplerian
orbits for each planet ({\bf S3}) and a 3-body dynamical model
({\bf S4}).  Tracking the dynamical evolution of both sets of
parameters in the future, we find that the two systems become unstable
in a few thousand years (Fig.\,\ref{F5}).  For the initial parameters
obtained with the orbital solution S3, the outer planet is lost after
only five thousand years, the same happening with the system S4 at
about forty thousand years.  This last solution is a slightly better
determination of the planetary system around {\small HD}\,202206, although
it is still very unsatisfactory.  It can nevertheless be used as a starting
point for a dynamical study of this system.

\subsection{Stable solutions}
\label{sec4.2}

Since the estimated age of the {\small HD}\,202206 star is about
5\,Gyr (Table\,\ref{T1}), it is  clear that the previous orbits are
not good.
One reason is that the fitted parameters
still present some uncertainties around the best fitted value.
This is particularly true
for the outer planet, with a small semi-amplitude variation of about
40~m/s.  Moreover, in order to fit our observational data to the
theoretical radial-velocity curve, we used the iterative
Levenberg-Marquardt method.  This method converges to a
minimum  $\chi^2$, but other close local minima may represent as
well a good fit for our data.  Additionally, there may exist additional
planets in the system that will also perturb the present solution.
We should thus consider that the set of parameters given in
section~\ref{orbsolutions}  constitutes the best determination
one can do so far, and we will  search
  for  more stable solutions in its  vicinity.

Starting with the orbital solution S4, obtained with the 3-body model
(Table\,\ref{T4}), we have searched  for possible nearby stable zones.
Since the orbit of the inner planet is well established,
with small standard errors,
we have kept the parameters of this planet constant.
We also did not change the inclination of the orbital planes, keeping
both at $90^\circ$.  For the outer planet we let $a$, $\lambda$,
$e$ and $\omega$ vary.  Typically, as in Fig.\,\ref{F6}
we have fixed $e$ and $\lambda$ to
specific values, and have spanned the $(a,\omega)$ plane of initial conditions
with a step size of  $0.005$ AU for $a$ and 1 degree for $\omega$.
For each initial condition, the orbit of the planets are integrated over
2000 years with  the  symplectic integrator SABAC4 of
Laskar and Robutel (2001), using a step size of $0.02$ year.
The stability of the orbit is then measured by
frequency analysis (Laskar, 1990, 1993). Practically, a refined
determination of the mean motion $n_2, n_2'$ of the outer planet
is obtained over two consecutive time interval of length $T=1000$ years,
and the measure of  the difference $D = \abs{n_2-n_2'}/T$
(in deg/yr${}^2$ in Fig.\,\ref{F6})
is a measure of the chaotic diffusion of the trajectory.
It should be close to zero for a regular solution and
high values will correspond to strong chaotic motion
(see Laskar, 1993 for more details).

In the present case a regular motion will require  $ D < 10^{-6}$.
We find that the vicinity of the {\small HD}\,202206 system is very
chaotic (light grey region of Fig.\,\ref{F6})
and the majority of the initial conditions will rapidly become
unstable.  Because of the two planets' proximity and large values of the  masses
and eccentricities, the chaotic behavior was expected.
We nevertheless find a small  region of initial conditions
(the darker region of  Fig.\,\ref{F6})
with very small diffusion and where the trajectories
 remain stable for several million years.
 These orbital solutions  correspond to the resonant
 island of  an orbital  5/1 mean motion resonance.

\begin{figure}[t!]
   \begin{tabular}{c}
    \includegraphics*[width=8.5cm]{Figures/ fig06.ps}
   \end{tabular}
  \caption{Global view of the dynamics of the {\small HD}\,202206
    system for variations of the perihelium and semi-major axes of the
    outer planet. Light grey areas correspond to high orbital diffusion
    (instability) and dark areas to low diffusion (stable orbits).
    The grey scale is the stability index ($D$) obtained through a frequency
    analysis of the longitude of the outer planet over two
    consecutive time intervals of 1000 yr.
    Labeled lines give the value of $ \sqrt{\chi^2} $ obtained for
    each choice of parameters. Initial conditions in the dark spot
    stable zone (with $\log_{10}(D) < -6$)
    are trapped in a 5/1 mean motion resonance.
    \llabel{F6}}
\end{figure}

Labeled lines of Figure~\ref{F6} give the value
of $\sqrt{\chi^2}$ obtained for each choice of parameters.
We observe that the minimum $\chi^2$  obtained for the present data is
effectively in a zone of high orbital diffusion.  Stable orbits can
only be found inside the dark spot, which corresponds to the 5/1 mean
motion resonance.
In order to find stable solutions
coherent with our data, we need to increase $\chi^2$ until we get
initial conditions inside this resonant zone.  Thus, the best fit that
provides a stable orbital solution will present $\sqrt{\chi^2} \sim
1.7$, which is still acceptable.  For instance, choosing
$\omega=55.50^\circ$ and $a=2.542$\,AU (solution {\bf S5}),
we have $\sqrt{\chi^2}=1.67$ (Table\,\ref{T5}).

\begin{table}[th!]
\caption{Stable orbital parameters for the two planets orbiting
{\small HD}\,202206. Using the orbital solution S4
(Table\,\ref{T4}), we chose the values of the perihelium and the
semi-major axes of the outer planet such that the system becomes
stable. The new system is in a $5/1$ mean motion resonance.}
\llabel{T5}
\begin{center}
\begin{tabular}{l l c c} \hline \hline
{\bf Param.}  & $ {\bf S5} $ & {\bf inner} & {\bf
outer}   \\ \hline
 $a$          & [AU]                 & $ 0.83040 $ & $ {\bf 2.54200} $ \\
 $\lambda$    & [deg]                & $ 266.22864 $ & $ 30.58643 $ \\
 $e$          &                      & $ 0.43492 $ & $ 0.26692 $ \\
 $\omega$     & [deg]                & $ 161.18256 $ & $ {\bf 55.50000 } $ \\
 $i$          & [deg]                & $ 90.00000 $ & $ 90.00000 $ \\
 $m $       & [M$_\mathsf{Jup}$]     & $ 17.42774 $ & $ 2.43653 $ \\ \hline
Date         & [JD-2400000]         & \multicolumn{2}{c}{52250.00}   \\
rms          & [m/s]                & \multicolumn{2}{c}{\bf 10.73}   \\
$\sqrt{\chi^2}$     &                      & \multicolumn{2}{c}{\bf 1.67}   \\ \hline
\end{tabular}
\end{center}
\end{table}

\begin{figure}[h]
   \begin{tabular}{c}
    \includegraphics*[width=8.5cm]{Figures/ fig07.ps}
   \end{tabular}
  \caption{In the orbital solution S5 (Table\,\ref{T5}),
  the resonant argument $\theta = \lambda_1 - 5 \lambda_2 +  g_1 \, t + 3 g_2 \, t$
  is in libration around $\theta_0 = 76.914$ deg, with a libration
period   $P_{\theta} \approx 19.4$ yr, and an amplitude of about $37$ degrees.
    \llabel{F7}}
\end{figure}

Henceforward, we will consider that  the solution S5
(with orbital parameters given in Table\,\ref{T5})
is more representative of the  real behavior of
the {\small HD}\,202206 planetary system.
Ideally, we would like that the best fit to the observation
would also be in a stable region, but we assume that in the present case,
this requirement is not satisfied because of the limited
time span and resolution of the observations that do not
allow us to solve precisely for the outer planet elements.
In particular, we have not been able yet to solve for the
mutual
inclination of the planets that may also shift the location of the regular
resonant island.

For the orbital solution S5, the main resonant argument is
\begin{equation}
\theta = \lambda_1 - 5 \lambda_2 +  g_1 \, t + 3 g_2 \, t
\end{equation}
where $g_1$ and $g_2$ are fundamental secular frequencies of the
system related to the perihelion of the inner and outer planet
respectively (see Laskar, 1990). Both are retrograde,  with periods
$P_{g_1} \approx 399000$ yr and $P_{g_2} \approx 339$ yr. The  resonant argument
$\theta$ is in libration around $\theta_0 = 76.914$ deg, with a libration
period   $P_{\theta} \approx 19.4$ yr, and an amplitude of about $37$ degrees
(Fig.\,\ref{F7}). It should be noted that for the real solution,
the libration amplitude may be smaller, but the libration period
will be of the same order of magnitude, that is around 20 years.
The observation of the system over a few additional years may
then provide an estimate of the libration amplitude and thus
a strong constraint on the parameters of the system.

\subsection{Secular evolution}

Using the S5 stable orbital parameters (Table\,\ref{T5}) we
have first integrated our
system over a few thousand years (Fig.\,\ref{F7}). Unlike
results plotted in Fig.\,\ref{F5} for unstable systems, we now observe
a regular variation of the eccentricity of both planets.

Because of the strong gravitational interactions with the inner
planet, the outer planet still shows large variations in its
orbital parameters.  The eccentricity can range from less than 0.1 to
about 0.45, while the semi-major axes varies between 2.3 and almost
3\,AU.  As a result, the minimum distance between the two planets'
orbits is only 0.4\,AU.  However, because of the  5/1
mean motion resonance trapping, the two planets never come closer than about
1.1\,AU.  We also observe rapid secular variations of the orbital
parameters, mostly driven by the rapid secular frequency
$g_2$, with a period $P_{g_2} \approx 339$ yr.   These secular variations of
the orbital elements are much faster than in our Solar System,
and should make possible their direct observation.

The S5 orbital parameters (determined using the  global view of the
system dynamics given by Figure~\ref{F6})
allow us to obtain an orbital evolution of the system
that is much  more satisfactory than the one
obtained by a direct orbital fit (section~\ref{orbsolutions}, solutions
S3 and S4), as the system now
remains stable within five thousand years (Figs.\,\ref{F5}
and~\ref{F7}).
Although from the previous stability analysis (section \ref{sec4.2})
we know that the stability of the orbit is granted for a much
longer time interval than the few thousand years of the
orbital integration, we have also directly tested
the stability of the system S5  over 5 Gyr.
The results displayed in Figure~\ref{F8} show
that indeed, the orbital elements  evolve in a
regular way, and  remain relatively stable over the age of the central star.

\begin{figure}[t!]
   \begin{tabular}{c}
    \includegraphics*[width=8.5cm]{Figures/ fig08.ps}
   \end{tabular}
  \caption{Dynamical evolution of the eccentricity with
    the orbital solution S5 (Table\,\ref{T5}). As expected, the
    eccentricity presents regular variations that contrasts to the
    irregular behavior of the orbital solutions presented in
    Fig.\,\ref{F5}. Due to the strong gravitational interactions, the
    secular variations of the eccentricity are rapid,
    and mostly driven by the secular frequency $g_2$,
    with period  $P_{g_2} \approx 339$ yr.
    \llabel{F8}}
\end{figure}

\begin{figure}[t!]
   \begin{tabular}{c}
    \includegraphics*[width=8.5cm]{Figures/ fig09a.ps} \\
    \includegraphics*[width=8.5cm]{Figures/ fig09b.ps}
   \end{tabular}
  \caption{Long term evolution of the semi-major axes and the eccentricity for
    both planets with the orbital solution S5
    (Table\,\ref{T5}). The system remained stable during 5 billion
    years. The small variation in the semi major axes and eccentricity
    around 2 Gyr is probably due to some very slow diffusion
    through a small resonance.
    \llabel{F9}}
\end{figure}

\section{Discussion and conclusion}

In this paper we report the presence of a second planet orbiting the
{\small HD}\,202206 star, whose orbital parameters are quite
unexpected.  This system was first described as a star orbited by a
massive planet or a light brown dwarf (Udry et al., 2002,
Paper\,I).  The first {\small CORALIE} measurements already suggested
the presence of a second, longer period companion, but it was thought
to be a very distant stellar companion.  The existence of a second,
much less massive body at only $2.55$\,AU, was
never observed and troubles our understanding of the hierarchy of
planetary systems.  Two other multiple planetary systems were
discovered with orbital periods identical to this one: {\small
  HD}\,12661 (264 and 1445 days) and {\small HD}\,169830 (226 and 2102
days).  However, the mass ratio of the two planets differ in both
cases by less than a factor of two, while for {\small HD}\,202206 this
ratio is almost ten.  Mazeh and Zucker (2003) suggested that a
possible correlation between mass ratio and period ratio in multiple
planetary systems may exist.  Using the multiple planetary systems
discovered to the date (including Jupiter and Saturn), they found
that, except for the 2/1 resonant systems, the correlation between the
logarithms of the two ratios was 0.9498. In order to keep this result,
the consideration of the present planetary system shows that
mean motion resonances other than the 2/1 should probably also
be excluded from the correlated systems.

These observations raise the question of how this system
was formed, bringing additional constraints to the existent theories.
Supposing that the inner body is effectively a brown dwarf, then the
new found planet will be an example of a planet in a binary, formed in
the circumbinary protoplanetary disk. This assumption seems to be a real
possibility, since recent numerical simulations show that a planet formed in a
circumbinary disk can migrate inward until it is captured in resonance (Nelson,
2003). Inversely, we can suppose that both companions were formed in the
accretion disk of the star, with the result that the inner planet is not a brown
dwarf.  This leads to the re-definition of the brown-dwarf limits and requires
that the initial disk around {\small HD}\,202206 was much more massive than we
would usually think.

Dynamically the system is very interesting and promising. The gravitational
interactions between the two planets are strong, but stability is possible due
to the presence of a 5/1 mean motion resonance with a libration period of about
20 years. This is the first observation of such an orbital configuration that may
have been reached through the dissipative process of planet migration
during the early stages of the system evolution.

The strong gravitational interactions among the planets
may also allow us to correctly
model their effect in the nearby future.  With the current
precision of {\small CORALIE}, fixed at about 8\,m/s for {\small
  HD}\,202206, we are presently close to detecting the trace of the
planet-planet interactions in data. This will be reached even sooner with
the higher precision measurements presently obtained with the {\small
ESO HARPS} spectrograph at a $\sim$\,1\,m/s level (Mayor et al., 2003).
The planet-planet interaction signature may provide
important information on the inclination of the orbital planes
and allow us to determine the mass values of both planets.

\paragraph{Acknowledgments} We are grateful to the staff from the Geneva
Observatory which maintains the 1.2-m Euler Swiss telescope and
the {\small CORALIE} echelle spectrograph at La Silla. This work was supported
by Geneva University, the Swiss NSF (FNRS) and from PNP-CNRS. A.C. also benefited
from the support of the HPRN-CT-2002-00308 European training network
programme.

\makeatletter \renewcommand\@biblabel[1]{} \makeatother

redpajama_set_name: RedPajamaArXiv


text:
Marge Cooney Was Married To Phil Donahue: Her Personal & Professional Details
Post category:Biography / Entertainment
Post last modified:September 18, 2020
Many of you might not have heard the name, Marge Cooney. Well, it's not surprising to hear as the first wife of TV personality Phil Donahue. The former couple was married for over a decade and became parents to five wonderful kids.
Upon separating, both of them started a new life with new people. While Phil still remains in the media spotlight, his ex-wife Marge is completely out of the picture.
Many tabloids suggest she is dead without proper evidence. Today let's find out about her whereabouts and also take a look at her marriage life with ex-hubby Phil.
Marge Cooney and Phil Donahue: Details on their wedding
After about a year of their engagement, Margie and Phil officially became one. They wedded on February 1st, 1958, in one of the oldest cathedrals on the US, San Felipe de Neri, New Mexico. It was a Solemn High Nuptial Mass, meaning there were three priests.
The ceremony in itself was relatively small with only a few of their friends and family in attendance.
Marge was first introduced to Phil by her brother
The former flames first met each other while studying at the University of Notre Dame. During his college days, Phil was quite into theatres. And by the virtue of theatre, he came across a man named Jim Cooney. Quickly, the two of them became close friends.
Around the same time, Jim introduced his sister Margaret Marge Cooney, a former Marquette University student, to the handsome Phil. While recalling the moment he first laid eyes on her, he described her as a tall, attractive girl who looked sexy in an overcoat buttoned up around her neck.
Soon the duo began dating, however, their relationship wasn't serious at first. Their real relationship didn't star until one day she quit school and moved to Chicago, while Phil was in his senior year. Back then, she had gotten a job at Price Waterhouse in the Prudential Building and the Loop.
Thankfully, the distance didn't discourage the young couple.
Marge Cooney and Phil Donahue became parents of five children
From their union that lasted over a decade, Margaret and Phil welcomed five kids, two of whom were born in the first year.
The TV show host was desperate to have kids. This is why he and his wife tried for children, a few months into their marriage. However, for the first few months, they didn't have any luck. Thankfully, after months of trying Marge became pregnant with their first child.
The Donahue family at the Ohio State Fair From left to right (Phil Donahue, Mary Rose, Mike, Dan, Kevin, Jim, and Margie.)
They welcomed their first son Michael Donahue on January 30, 1959. He was born prematurely. Besides, Michael has been married to Martha Reed von Gal.
In the same year of 1959, Marge gave birth to their second child, Kevin Donahue on 9th December 1959.
Subsequently, in a matter of three years, Marge gave birth to two more sons Daniel Donahue and James Patrick, born 1963. After welcoming four sons, the couple became parents to their one and only daughter, Mary Rose Donahue in 1965.
Unfortunately, Marge's youngest son, James 'Jim' died at the age of 51 in 2014. He used to live in Hawaii and practiced law.
Marge and Phil separated in 1973, reconciled, and divorced
In the summer of 1973, the pair decided to go their separate ways. Consequently, Marge moved back to her hometown of Albuquerque with her two kids and rented an apartment there. The other three children were left in Phil's care.
From Left to Right (Jim, Kevin, Phil, Dan, Mike) in an event.
They remained separated for ten-months before getting back together. Cooney and Phil did it for the sake of their five kids. Nevertheless, things didn't go well and after four-months of reconciliation, they separated for good.
In 1975, divorce between the two finalized and Phil got the sole custody of his four sons while their daughter Mary was left in the care of her mother.
Marge and Phil both later remarried
After divorcing the Phil Donahue show star, Margie married again and soon moved back to her native, New Mexico. She had completely disappeared from the public. The only time public was able to see her is when Phil added a family picture with Marge and their five kids in his book, Phil Donahue, My Own Story (1980).
After separation from Cooney, Phill exchanged vows with Marlo Thomas on May 21st, 1980. The pair do not share any children, even so, she became the step-mom of Phil's five kids, now four.
In the year 2020, on the occasion of their 40th wedding anniversary, Phil and Marlo released a book titled, What Makes a Marriage Last.
Where is Marge Cooney these days? Is she dead or alive?
Well, there are varied reports regarding Marge's current whereabouts. Numerous tabloids claim Cooney passed away in 2018, however, the information that they have written about is of a different woman who happened to have the same name as Margie.
Now talking about her actual whereabouts, well, it is still a mystery. She did move back to her native place of Albuquerque, New Mexico upon divorcing Phil, and since then, she has kept a low profile.
Despite all that, Marge is alive and well. She is not dead as many outlets suggest. She is currently 82-years-old and lives a peaceful life.
How much is Marge Cooney's net worth?
There is no record of Marge's professional life which makes it quite difficult to find out about her total fortune. Nonetheless, she must've gotten a terrific amount of divorce alimony from her famous spouse, who in the 70s, was earning upwards of $15,000 a year.
As of 2020, Marge's ex-husband Phil has a staggering net worth of $150 million.
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text: Alice is currently a sophomore and was first exposed to programming in freshman year, when she took a Java Programming course at her school. She started gaining interest in programming and developed a game to help people of all ages in topics such as health and the human body. Although this was her first experience programming, she had been exposed to the lack of girls in STEM fields since elementary school. In several instances, she was greatly outnumbered by boys in competitions and other places. However, she did not let this faze her and continued pursuing her interests in male-dominated areas such as engineering and mathematics. Currently, her strongest passion is chemistry, and she hopes to apply and contribute her knowledge in computing to biochemistry research. In the future, she also aims to develop artificial intelligence that will be able to detect major chromosomal abnormalities early in pregnancy, or robots and programs that can detect rapid senescence that may lead to clues about Alzheimer's Disease in its early stages. Aside from computing, Alice enjoys swimming. During her freshman year, she was on her school's JV swim team and currently holds the league record for 50 butterfly and the 4x100 freestyle relay. She now swims on the varsity team, and also enjoys playing French horn and dancing.


The BET Experience Weekend has officially begun and Miss Diddy & CMPR Inc. held the Party of the Evening last night at the Annual "Toast To Young Hollywood" Affair with folks like Meek Mill, Russell Simmons and More stopping through.
Keep an eye out for India Love if you don't know about her already… she's stopping hearts of both Male and Females alike.
One Step Closer Foundation's Celebrity Poker Tournament Held at Planet Hollywood in Vegas brought out some Great Folks for a Great Cause.
All in support of the Foundation and their Founder, Jacob Zalewski, a Great and Brave Man who's Life and Achievements have gained himself the Respect of Many for Years. How could the Heavy Hitters NOT Support Jacob and his cause to Help those with Cerebral Palsy.
The event brought out Montel Williams, Cheryl Hines of "Curb Your Enthusiasm", Jennifer Tilly and More… Even Mr. Belding a.k.a. Dennis Haskins and WWF's Alicia Webb came out to Support the Cause over a Game of Cards.
And the Best part of the Night was Jennifer Braff sharing her Beauty and Laker Sized People Skills in Hosting the Event.
Nothing ever lasts. For some of you this might be good news but it's been long enough that it looks like Big Sean and Ariana Grande are never, ever, ever getting back together. The couple had been dating since October 2014 during which time Sean made it his mission in life that Grande would never have to walk, so that a child may live. Sadly, the two were unable to reconcile whatever issues they had as a couple and have made the decision to undertake a conscious uncoupling as they both prepare for their 2015 tours.
A source revealed that their conflicting touring schedules and lack of available time together over the next year prompted the split. "They both deeply care for each other and remain close friends," the pair's reps said in a joint statement. At least, this is the official line they're feeing the media. She's definitely getting over it quickly with news gossip sprouting up that the "Love Me Harder" songstress has been canoodling with Niall Horan of One Direction. Grande has however got on record with multiple outlets adamantly stating that her business is her business and that love life has no bearing on her identity. "I am tired of living in world where women are mostly referred to as a man's past, present or future PROPERTY / POSSESSION," said Grande on Instagram.
Judging from the rumors it seems like there's plenty of blame to go around for the couple with accounts ranging from Ariana's ballooning, out-of-control ego to both partners experimenting with how much greener the grass really is on the other side. The Daily Mail reports that some have questioned whether or not the split was to do with Grande's friendly relationship with fellow 21-year-old pop star Justin Bieber or if Big Sean's own bad habits die hard. We're guessing a little bit of both?
The news of the couple's split in late April comes as no surprise to anyone as rumors had be swirling about trouble in paradise for months. SugarScape reported back in January that the 27-year-old "IDGAF" rapper had been stepping out on Ms. Grande by having an affair with a popular Instagram model. Big Sean might have forgotten that sexting studies show that 60% of people sending or receiving sexts keep those things saved on their devices. You think the rapper might learn the first time after his 2014 engagement to Naya Rivera was called off as a direct results of Rivera learning of Sean's screaming infidelities.
Big Sean's third album, "Dark Sky Paradise," was released in early 2015 and helped Sean achieve his first number one spot in the Billboard top 200. Grande is set for a role in the upcoming Fox horror anthology series, "Scream Queens" to premier this September. She will be joined by Emma Roberts, Nick Jonas and the original scream queen herself, Jamie Lee Curtis.
Omar Alhindi is an 18 Year Old Musical Prodigy.. A Singer & Songwriter who also Produces his own Music.
If you haven't heard of him yet, you will get to know him soon enough. His musical abilities are like that of the few in music greatly gifted with a fusion of all genres to create their own unique and distinct style and sound.
And of course we may have a bit something to do with it… but you Won't Be Sorry… Check out Omar gettin his Hollywood Swag on at Sham Ibrahim's Celeb Selfie Portrait Art Gallery with Bizzy Bone, Maitland Ward and Jeffery Exclusive.
Courtney Stodden showed up to Sham Ibrahim's Art Gallery for his Celeb Selfie Portrait Series Yesterday at "Sweet!" in The Hollywood & Highland Mall.
Like the other Celebrity Guests who attended Sham's Gallery… Courtney had her own Celeb Selfie Portrait that was presented to her by the Artist Himself, Sham.


Why entrepreneurial thinking, acting and communicating are important to me and how I deal with "Entrepreneurial Storytelling" in research-based teaching I tell about and reflect upon in the Lifelong Learning Blog of the PHZH.
This blog article is in German only! – The German title is: "Durch forschungsbasierte Lehre zum Entrepreneurial Storyteller werden".


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Retail winner to rendezvous in Chicago
Hobart business owner Lucy Given has been named as the first ever Retailer of the Year winner in the Gift and Life Instyle Awards (GALA) and will go on to represent Australia in Chicago at the IHA Global Innovation Awards this March.
Lucy created LUC. design in 2013, drawing on her 25 years' experience in both commercial and residential interior design and retail. Now the design store offers those in Tasmania a go-to source for interesting, iconic and well-designed products.
"Tasmania is a small state and it is always a challenge in any retail environment to be competitive and unique," Lucy says.
"It is such an honour to have achieved national recognition and be able to represent Australia."
The IHA Global Innovation Awards (GIA) were created as a means of fostering innovation and excellence in housewares retailing around the word. LUC. design store will be one of the national winners nominated for the awards, judged by an internationally acclaimed panel of retail experts.
LUC. design store will also be recognised among other great Australian brands and stores at the annual Gift and Life Instyle Awards night, held at the end of day one of the five-day Reed Gift Fairs Sydney event.
"The Gift and Life Instyle (GALA) awards have helped my business and its growth, along with providing a platform to be able to inspire people to love great design and make beautiful homewares part of one's everyday life."
Top marks for new University College approach
Pathway to a healthier state