In late 2003, the young eruptive variable star V1647 Orionis optically brightened by over 5 mag, stayed bright for around 26 months, and then declined to its pre-outburst level. In 2008 August, the star was reported to have unexpectedly brightened yet again and we herein present the first ...
有没有比V1647 Orionis更年轻的恒星?探索宇宙2024-07-28 07:14:16 知识大剧场 广东 举报 0 分享至 0:00 / 0:00 速度 洗脑循环 Error: Hls is not supported. 视频加载失败 声明:个人原创,仅供参考 知识大剧场 147粉丝 热爱生活,喜欢发明。 05:45 荷兰美女爱上中国小伙,追到中国后慌了:这不是...
Our observations show that over the past four and a half years, V1647 Ori and region C near the Herbig-Haro object HH 22A have been undergoing a slow dimming at a rate of ~0.04magyr–1 and ~0.05magyr–1, respectively, in R band, which is six times slower than the rate during a ...
V1647 ORIONIS: ONE YEAR INTO QUIESCENCEdoi:10.1088/0004-6256/135/1/423Colin AspinTracy L. BeckBo ReipurthIOP Publishing
V1647 Orionis underwent an FU Ori kind of outburst in 2004 and returned to its pre-outburst phase in early 2006. Within just 2 years it again underwent a second outburst in 2008; such an event is rarely seen in FU Ori type of outburst. We therefore followed the source in its second ...
Post‐outburst phase of McNeil’s nebula (V1647 Orionis)[J] . D. K.Ojha,S. K.Ghosh,A.Tej,R. P.Verma,S.Vig,G. C.Anupama,D. K.Sahu,P.Parihar,B. C.Bhatt,T. P.Prabhu,G.Maheswar,H. C.Bhatt,B. G.Anandarao,V.Venkataraman.Monthly Notices of the Royal Astronomical Society ....
High Cadence Time-Series Photometry of V1647 OrionisFabienne A. BastienK. G. StassunD. A. WeintraubAmerican Astronomical Society Meeting Abstracts #215
V1647 Orionis underwent an FU Ori kind of outburst in 2004 and returned to its pre-outburst phase in early 2006. Within just 2 years it again underwent a second outburst in 2008; such an event is rarely seen in FU Ori type of outburst. We therefore followed the source in its second ...
doi:10.1093/PASJ/57.1.203Devendra OjhaNobuhiko KusakabeMotohide TamuraYasushi NakajimaMisato FukagawaKoji SugitaniDaisuke BabaDaisuke KatoMikio KuritaChie NagashimaAstronomical Society of Japan
Therefore, the photometric and spectroscopic monitoring ofthe post-outburst phase of these objects is required to settle the classof eruptive variables to which they belong. V1647 Ori had gone intooutburst phase in early 2004 (McNeil 2004) and faded considerablyaroundlate2005(Ojhaetal. 2006). It...