scholarly journals The Unusual Evolutionary State of Nova Scorpii 1994

2002 ◽  
Vol 187 ◽  
pp. 373-378
Author(s):  
Christopher A. Tout ◽  
Enikő Regős ◽  
Dayal Wickramasinghe
Keyword(s):  
Black Hole ◽  
Main Sequence ◽  
Main Sequence Star ◽  
Chemical Pollution ◽  
Evolutionary Status ◽  
Low Velocity ◽  
Alternative Scenario ◽  
X Ray ◽  
The Core ◽  
Evolutionary State

AbstractWe have investigated possible models for the evolutionary status of the black-hole soft X-ray transient Nova Scorpii. We propose that it is a main-sequence star in which convective overshooting, or some equivalent mixing, occurs at the core-envelope boundary. Recent detections of chemical pollution on the surface of the secondary suggest that the black hole formed in a supernova whose ejecta left and fell back at a sufficiently low velocity to accrete on to the secondary. We examine the effects of increased opacity, increased metallicity and reduced hydrogen abundance on the evolution of the secondary in the hope that these might lead to an alternative scenario. All these only exacerbate the problem.

scholarly journals Some Aspects of the Evolutionary Status Of W Ursae Majoris Binaries Deduced from Observational Data

1982 ◽  
Vol 69 ◽  
pp. 301-304
Author(s):  
Walter Van Hamme
Keyword(s):  
Observational Data ◽  
Spectral Type ◽  
Main Sequence ◽  
Type A ◽  
Type Systems ◽  
Primary Component ◽  
Main Sequence Star ◽  
Evolutionary Status ◽  
Evolutionary Stage ◽  
Evolutionary State

AbstractWe have developed a test for the evolutionary state of W Ursae Majoris binaries by comparing the observed spectral type of 31 of these systems (14 of type W and 17 of type A) with the expected one when their primary component is an unevolved main sequence star. It appears that both the W- and A-type systems have a primary with a mass and radius too large to be compatible with the observed spectral type,so there is no indication that each type should mark a different evolutionary stage.

scholarly journals Slow decline and rise of the broad [O iii] emission line in globular cluster black hole candidate RZ2109

2019 ◽  
Vol 489 (4) ◽  
pp. 4783-4790 ◽  
Author(s):  
Kristen C Dage ◽  
Stephen E Zepf ◽  
Arash Bahramian ◽  
Jay Strader ◽  
Thomas J Maccarone ◽  
...  
Keyword(s):  
Black Hole ◽  
Emission Line ◽  
Globular Clusters ◽  
X Ray ◽  
Hydrogen Emission ◽  
Black Hole Candidate ◽  
The Core ◽  
Spectroscopic Monitoring ◽  
Slow Decline ◽  
Over Time

ABSTRACT RZ2109 is the first of several extragalactic globular clusters shown to host an ultraluminous X-ray source. RZ2109 is particularly notable because optical spectroscopy shows it has broad, luminous [O iii] λλ4959,5007 emission, while also having no detectable hydrogen emission. The X-ray and optical characteristics of the source in RZ2109 make it a good candidate for being a stellar mass black hole accreting from a white dwarf donor (i.e. an ultracompact black hole X-ray binary). In this paper we present optical spectroscopic monitoring of the [O iii]5007 emission line from 2007 to 2018. We find that the flux of the emission line is significantly lower in recent observations from 2016 to 2018 than it was in earlier observations in 2007–2011. We also explore the behaviour of the emission line shape over time. Both the core and the wings of the emission line decline over time, with some evidence that the core declines more rapidly than the wings. However, the most recent observations (in 2019) unexpectedly show the emission line core rebrightening

scholarly journals GRB 101225A - a new class of GRBs?

2011 ◽  
Vol 7 (S279) ◽  
pp. 91-94
Author(s):  
C. C. Thöne ◽  
A. de Ugarte Postigo ◽  
C. Fryer ◽  
K. Page ◽  
J. Gorosabel ◽  
...  
Keyword(s):  
Neutron Star ◽  
Main Sequence ◽  
Main Sequence Star ◽  
Thermal Component ◽  
X Ray ◽  
New Class ◽  
Faint Galaxy ◽  
Long Duration ◽  
New Type ◽  
Near Future

AbstractThe Christmas burst, GRB 101225A, was one of the most controversial bursts in the last few years. Its exceptionally long duration but bright X-ray emission showing a thermal component followed by a strange afterglow with a thermal SED lead to two different interpretations. We present here our model ascribing this strange event to a new type of GRB progenitor consisting of a neutron star and an evolved main-sequence star in a very faint galaxy at redshift 0.33 while Campana et al. (2011) proposed a Galactic origin. New observations at several wavelengths might resolve the question between the two models in the near future.

scholarly journals A LOW-MASS MAIN-SEQUENCE STAR AND ACCRETION DISK IN THE VERY FAINT X-RAY TRANSIENT M15 X-3

2015 ◽  
Vol 807 (1) ◽  
pp. 52 ◽  
Author(s):  
R. M. Arnason ◽  
G. R. Sivakoff ◽  
C. O. Heinke ◽  
H. N. Cohn ◽  
P. M. Lugger
Keyword(s):  
Accretion Disk ◽  
Main Sequence ◽  
Main Sequence Star ◽  
X Ray ◽  
Low Mass

scholarly journals V2282 Sgr Revisited

2014 ◽  
Vol 1 (1) ◽  
pp. 118-122
Author(s):  
Roberto Nesci ◽  
Corinne Rossi ◽  
Antonio Frasca ◽  
Ettore Marilli ◽  
Paolo Persi ◽  
...  
Keyword(s):  
Light Curve ◽  
Accretion Disk ◽  
Main Sequence ◽  
Optical Spectra ◽  
Emission Lines ◽  
Main Sequence Star ◽  
Strong Emission ◽  
X Ray ◽  
Type Spectrum

The nature of V2282 Sgr is examined on the basis of several multiband observations: a 20 years long I-band light curve of V2282 Sgr obtained from archive photographic plates of the Asiago and Catania Observatories; a CCD R-band light curve obtained at Cornero Observatory; JHK photometry from 2MASS and UKDISS; <em>Spitzer</em> IRAC and MIPS images; optical spectra from Loiano Observatory; X-ray flux from <em>CHANDRA</em>. The star has a K-type spectrum with strong emission lines and is irregularly variable at all wavebands. The overall evidences suggest that V2282 Sgr is a Pre Main Sequence star with an accretion disk.

ON THE THEORY OF GAMMA RAY BURSTS AND HYPERNOVAE: THE BLACK HOLE SOFT X-RAY TRANSIENT SOURCES

2003 ◽  
Vol 18 (04) ◽  
pp. 527-576 ◽  
Author(s):  
CHANG-HWAN LEE ◽  
GERALD E. BROWN
Keyword(s):  
Mass Transfer ◽  
Black Hole ◽  
Mass Loss ◽  
Evolutionary History ◽  
Main Sequence ◽  
Gamma Ray ◽  
Supernova Explosion ◽  
Sequence Evolution ◽  
X Ray ◽  
Black Hole Binaries

We show that a common evolutionary history can produce the black hole binaries in the Galaxy in which the black holes have masses of ~ 5 - 10M⊙. In the black hole binaries with low-mass, ≲ 2.5M⊙ ZAMS (zero age main sequence) companions, the latter remain in main sequence during the active stage of soft X-ray transients (SXT's), most of them being of K or M classification. In two intermediate cases, IL Lupi and Nova Scorpii with ZAMS ~ 2.5M⊙ companions the orbits are greatly widened because of large mass loss in the explosion forming the black hole, and whereas these companions are in late main sequence evolution, they are close to evolving. Binaries with companion ZAMS masses ≳ 3M⊙ are initially "silent" until the companion begins evolving across the Herzsprung gap. We provide evidence that the narrower, shorter period binaries, with companions now in main sequence, are fossil remnants of gamma ray bursters (GRB's). We also show that the GRB is generally accompanied by a hypernova explosion (a very energetic supernova explosion). We further show that the binaries with evolved companions are good models for some of the ultraluminous X-ray sources (ULX's) recently seen by Chandra in other galaxies. The great regularity in our evolutionary history, especially the fact that most of the companions of ZAMS mass ≲ 2.5M⊙ remain in main sequences as K or M stars can be explained by the mass loss in common envelope evolution to be Case C; i.e. to occur only after core He burning has finished. Since our argument for Case C mass transfer is not generally understood in the community, we add an appendix, showing that with certain assumptions which we outline we can reproduce the regularities in the evolution of black hole binaries by Case C mass transfer.

scholarly journals Are there pre-main-sequence/black hole X-ray binaries?

2018 ◽  
Vol 480 (3) ◽  
pp. 3856-3863
Author(s):  
Xiao-Tian Xu ◽  
Xiang-Dong Li
Keyword(s):  
Black Hole ◽  
Main Sequence ◽  
X Ray ◽  
X Ray Binaries

scholarly journals Gaia’s detectability of black hole–main sequence star binaries formed in open clusters

2020 ◽  
Vol 72 (3) ◽  
Author(s):  
Minori Shikauchi ◽  
Jun Kumamoto ◽  
Ataru Tanikawa ◽  
Michiko S Fujii
Keyword(s):  
Black Hole ◽  
Main Sequence ◽  
Star Clusters ◽  
Interstellar Extinction ◽  
Open Clusters ◽  
Main Sequence Star ◽  
Chemical Abundance ◽  
Good Test ◽  
Orbital Periods ◽  
Chemical Anomalies

Abstract Black hole–main sequence star (BH–MS) binaries are one of the targets of future data releases of the astrometric satellite Gaia. They are supposed to be formed in two main sites: a galactic field and star clusters. However, previous work has never predicted the number of BH–MS binaries originating in the latter sites. In this paper we estimate the number of BH–MS binaries formed in open clusters and detectable with Gaia based on the results of N-body simulations. By considering interstellar extinction in the Milky Way and observational constraints, we predict that ∼10 BH–MS binaries are observable. We also find that chemical abundance patterns of companion MSs will help us to identify the origin of the binaries as star clusters. Such MSs are not polluted by outflows of the BH progenitors, such as stellar winds and supernova ejecta. Chemical anomalies might be a good test to confirm the origin of binaries with relatively less massive MSs (≲5 M⊙), short orbital periods (∼1.5 yr), and higher eccentricities (e ≳0.1).

scholarly journals The mass of the black hole in the X-ray binary M33 X-7 and the evolutionary status of M33 X-7 and IC 10 X-1

2009 ◽  
Vol 53 (3) ◽  
pp. 232-242 ◽  
Author(s):  
M. K. Abubekerov ◽  
E. A. Antokhina ◽  
A. I. Bogomazov ◽  
A. M. Cherepashchuk
Keyword(s):  
Black Hole ◽  
Evolutionary Status ◽  
X Ray ◽  
Ic 10

scholarly journals Comment on “A noninteracting low-mass black hole–giant star binary system”

Science ◽  
2020 ◽  
Vol 368 (6491) ◽  
pp. eaba3282 ◽  
Author(s):  
Ed P. J. van den Heuvel ◽  
Thomas M. Tauris
Keyword(s):  
Black Hole ◽  
Main Sequence ◽  
Close Binary ◽  
Main Sequence Stars ◽  
Solar Mass ◽  
Giant Star ◽  
X Ray ◽  
Low Mass ◽  
Red Giant ◽  
Star Binary

Thompson et al. (Reports, 1 November 2019, p. 637) interpreted the unseen companion of the red giant star 2MASS J05215658+4359220 as most likely a black hole. We argue that if the red giant’s mass is ~1 solar mass, its companion can be a close binary consisting of two main-sequence stars. This would explain why no x-ray emission is detected from the system.

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