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This article is or was the subject of a Wiki Education Foundation-supported course assignment. Further details are available on the course page. Student editor(s): Tiakortman.
Above undated message substituted from Template:Dashboard.wikiedu.org assignmentbyPrimeBOT (talk) 23:18, 16 January 2022 (UTC)[reply]
The topic discussed is a rare case. The original Helium stars were class B stars. Said: Rursus (☻) 21:02, 20 October 2008 (UTC)[reply]
Bibliography
!. http://science.sciencemag.org.ezproxy.pvc.maricopa.edu/content/347/6226/1126 - talk about HVS star 2. http://ic.galegroup.com.ezproxy.pvc.maricopa.edu/ic/scic/AcademicJournalsDetailsPage/AcademicJournalsDetailsWindow?disableHighlighting=&displayGroupName=Journals&docIndex=&source=&prodId=&mode=view&limiter=&display-query=&contentModules=&action=e&sortBy=&windowstate=normal&currPage=&dviSelectedPage=&scanId=&query=&search_within_results=&p=SCIC&catId=&u=mcc_pv&displayGroups=&documentId=GALE%7CA377862230&activityType=BasicSearch&failOverType=&commentary= 3. http://ky5ry5jk2j.search.serialssolutions.com/?ctx_ver=Z39.88-2004&ctx_enc=info%3Aofi%2Fenc%3AUTF-8&rfr_id=info%3Asid%2Fsummon.serialssolutions.com&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rft.genre=article&rft.atitle=The+unusual+%CE%B3-ray+burst+GRB+101225A+from+a+helium+star%2Fneutron+star+merger+at+redshift+0.33&rft.jtitle=Nature&rft.au=Th%C3%B6ne%2C+C.+C&rft.au=de+Ugarte+Postigo%2C+A&rft.au=Fryer%2C+C.+L&rft.au=Page%2C+K.+L&rft.date=2011-11-30&rft.issn=0028-0836&rft.eissn=1476-4687&rft.volume=480&rft.issue=7375&rft.spage=72&rft.epage=74&rft_id=info:doi/10.1038%2Fnature10611&rft.externalDBID=n%2Fa&rft.externalDocID=10_1038_nature10611¶mdict=en-US — Preceding unsigned comment added by Tiakortman (talk • contribs) 07:04, 15 February 2018 (UTC)[reply]
Discoveries of Helium stars- "GALEX J184559.8−413827 (or J1845−4138 for short), was initially classified as a faint helium-rich "hot subdwarf," but new spectroscopic observations reveal that this star is more hydrogen-deficient than previously thought."[1] This was in 2011 and was labeled a "hot subdwarf." This means that GALEX J184559.8-413827 is characterized with being hotter and larger than the sun, while also being completely devoid of hydrogen. From these classifications, this hot subdwarf is considered to be a extreme helium star. In South Africa, the Southern Africa Large Telescope (SALT) has been monitoring this massive helium star's high-resolution spectrum.
A Hypervelocity star (HVSs) called US 708, HVS 2 has been labeled a helium star. Being the most fast rotator, it is thought to be a remnant of a thermonuclear supernova.[2]
Origin of Helium stars After a binary mass transfer, a helium star is formed.[3]
Turning into a supernova The star will begin to grow in radius and evolve upon exploding into a supernova.[4]
Merging with a helium star Often when a supernova dies, long gamma ray bursts are emitted. In 2010 it was observed that the aftermath of a supernova death caused a helium star to merge with a neuron star. This led to the merger going through a common envelope phase (losing it's hydrogen) and emitting gamma ray bursts. [5]
References
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I don't know if this exists in the literature, but as the article compares the "He MS" to the main sequence per se, wouldn't it be useful to present an HR-type diagram showing the helium main sequence, especially as compared to the normal/hydrogen one? Or failing that, some statement clarifying how they relate. 109.255.211.6 (talk) 17:41, 31 May 2022 (UTC)[reply]
