scholarly journals Chemical abundances of secondary stars in low mass X-ray binaries

2006 ◽  
Vol 2 (S238) ◽  
pp. 43-48
Author(s):  
Jonay I. González Hernández ◽  
Rafael Rebolo ◽  
Garik Israelian
Keyword(s):  
Galactic Plane ◽  
Supernova Explosion ◽  
Compact Objects ◽  
Chemical Abundances ◽  
Mixing Processes ◽  
X Ray ◽  
Element Abundances ◽  
Supernova Explosions ◽  
Low Mass ◽  
X Ray Binaries

AbstractLow mass X-ray binaries (LMXBs) offer us an unique opportunity to study the formation processes of compact objects. Secondary stars orbiting around either a black hole or a neutron star could have captured a significant amount of the ejected matter in the supernova explosions that most likely originated the compact objects. The detailed chemical analysis of these companions can provide valuable information on the parameters involved in the supernova explosion such us the mass cut, the amount of fall-back matter, possible mixing processes, and the energy and the symmetry of the explosion. In addition, this analysis can help us to find out the birth place of the binary system. We have measured element abundances of secondary stars in the LMXBs A0620–00, Cen X-4, XTE J1118+480 and Nova Sco 94. We find solar or above solar metalicity for all these systems, what appears to be independent on their locations with respect to the Galactic plane. A comparison of the observed abundances with yields from different supernova explosion together with the kinematic properties of these systems suggest a supernova origin for the compact objects in all of them except for A0620–00, for which a direct collapse cannot be discarded.

scholarly journals Evolution of binaries with compact objects in globular clusters

2014 ◽  
Vol 10 (S312) ◽  
pp. 203-212
Author(s):  
Natalia Ivanova
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Neutron Stars ◽  
Globular Clusters ◽  
Compact Objects ◽  
Stellar Systems ◽  
Stellar Objects ◽  
X Ray ◽  
Low Mass ◽  
X Ray Binaries

AbstractDynamical interactions that take place between objects in dense stellar systems lead to frequent formation of exotic stellar objects, unusual binaries, and systems of higher multiplicity. They are most important for the formation of binaries with neutron stars and black holes, which are usually observationally revealed in mass-transferring binaries. Here we review the current understanding of compact object's retention, of the metallicity dependence on the formation of low-mass X-ray binaries with neutron stars, and how mass-transferring binaries with a black hole and a white dwarf can be formed. We discuss as well one old unsolved puzzle and two new puzzles posed by recent observations: what descendants do ultra-compact X-ray binaries produce, how are very compact triples formed, and how can black hole low-mass X-ray binaries acquire non-degenerate companions?

scholarly journals On obtaining neutron star mass and radius constraints from quiescent low-mass X-ray binaries in the Galactic plane

2018 ◽  
Vol 479 (3) ◽  
pp. 3634-3650 ◽  
Author(s):  
Alessio Marino ◽  
N Degenaar ◽  
T Di Salvo ◽  
R Wijnands ◽  
L Burderi ◽  
...  
Keyword(s):  
Neutron Star ◽  
Galactic Plane ◽  
X Ray ◽  
Star Mass ◽  
Neutron Star Mass ◽  
Low Mass ◽  
X Ray Binaries

scholarly journals A strange star scenario for the formation of isolated millisecond pulsars

2020 ◽  
Vol 633 ◽  
pp. A45 ◽  
Author(s):  
Long Jiang ◽  
Na Wang ◽  
Wen-Cong Chen ◽  
Xiang-Dong Li ◽  
Wei-Min Liu ◽  
...  
Keyword(s):  
Neutron Star ◽  
Galactic Plane ◽  
Critical Mass ◽  
Strange Star ◽  
Millisecond Pulsars ◽  
X Ray ◽  
Mass Distributions ◽  
The Galaxy ◽  
Low Mass ◽  
X Ray Binaries

According to the recycling model, neutron stars in low-mass X-ray binaries were spun up to millisecond pulsars (MSPs), which indicates that all MSPs in the Galactic plane ought to be harbored in binaries. However, about 20% Galactic field MSPs are found to be solitary. To interpret this problem, we assume that the accreting neutron star in binaries may collapse and become a strange star when it reaches some critical mass limit. Mass loss and a weak kick induced by asymmetric collapse during the phase transition (PT) from neutron star to strange star can result in isolated MSPs. In this work, we use a population-synthesis code to examine the PT model. The simulated results show that a kick velocity of ∼60 km s−1 can produce ∼6 × 103 isolated MSPs and birth rate of ∼6.6 × 10−7 yr−1 in the Galaxy, which is approximately in agreement with predictions from observations. For the purpose of comparisons with future observation, we also give the mass distributions of radio and X-ray binary MSPs, along with the delay time distribution.

scholarly journals Measuring the Masses of Compact Objects in Low-Mass X-Ray Binaries

2004 ◽  
Vol 194 ◽  
pp. 214-214
Author(s):  
Dawn M. Gelino
Keyword(s):  
Black Hole ◽  
Neutron Star ◽  
Compact Object ◽  
Compact Objects ◽  
Orbital Inclination ◽  
X Ray ◽  
Secondary Star ◽  
Low Mass ◽  
The Masses ◽  
X Ray Binaries

Low-mass X-ray binaries (LMXBs) contain compact, black hole (BH) or neutron star (NS) primaries, and cool, low-mass secondary stars. We measure the orbital inclination of the system in quiescence by modeling infrared (IR) ellipsoidal variations from the secondary star in order to determine the compact object mass. I present our results for a few LMXBs, including the first BH that appears to conclusively fall in the 3-5 M⊙ range.

scholarly journals Low-Mass X-Ray Binaries in the LMC

1987 ◽  
Vol 93 ◽  
pp. 689-689
Author(s):  
M.W. Pakull ◽  
K. Beuermann ◽  
L.P. Angebault ◽  
L. Bianchi
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Interstellar Medium ◽  
Compact Objects ◽  
X Rays ◽  
X Ray ◽  
Black Hole Candidate ◽  
Low Mass ◽  
X Ray Binaries

AbstractWe report results on three low-mass X-ray binaries (LMXB) in the LMC, obtained with EXOSAT, IUE and ground-based (ESO) telescopes: LMC X-2 which appears to be “Sco X-l”-like, LHG 83 and LHG 87. The latter are two weaker sources first detected in the course of the HEAO-B LMC survey. They have faint optical counterparts of which LHG 87 was only recently identified by us. In X-rays, they are characterized by ultrasoft X-ray spectra possibly characteristic of black-hole primaries. LHG 83 furthermore shows evidence for X-ray ionization of the surrounding interstellar medium, similar to the He III region around the black-hole candidate LMC X-l. X-ray binaries with masses of compact objects in excess of 3 M⊙ and ultrasoft X-ray spectra are comparatively frequent in the LMC. We suggest that subcritical accretion onto black holes takes place in LHG 83 and LHG 87.

scholarly journals Pulsational Instability of Accretion Disks around Compact Objects

1993 ◽  
Vol 134 ◽  
pp. 361-364
Author(s):  
T. Okuda ◽  
S. Mineshige
Keyword(s):  
Accretion Disks ◽  
Cataclysmic Variables ◽  
Compact Object ◽  
Linear Analysis ◽  
Compact Objects ◽  
Periodic Oscillations ◽  
X Ray ◽  
Axisymmetric Perturbation ◽  
Low Mass ◽  
X Ray Binaries

AbstractLinear analysis shows that radial oscillations in accretion disks around compact object are overstable to axisymmetric perturbation under a variety of conditions. Furthermore, numerical simulations confirm that the radial oscillations induce quasi-periodic modulations of the disk luminosity. The disk oscillation model may be responsible for quasi-periodic oscillations (QPOs) observed in low mass X-ray binaries (LMXBs), cataclysmic variables (CVs), and other compact objects.

scholarly journals The kHz QPOs of Neutron Stars and Millisecond Pulsars and Implications

2012 ◽  
Vol 8 (S290) ◽  
pp. 381-385
Author(s):  
Chengmin Zhang ◽  
Dehua Wang
Keyword(s):  
Magnetic Field ◽  
Low Frequency ◽  
Compact Objects ◽  
Periodic Oscillations ◽  
Disk Thickness ◽  
X Ray ◽  
Low Mass ◽  
Millisecond Timing ◽  
X Ray Binaries ◽  
Z Sources

AbstractThe kilohertz quasi-periodic oscillations (kHz QPOs) have been found in neutron star low mass X-ray binaries (NS-LMXBs), which present the millisecond timing phenomena close to the surface of the compact objects. We briefly summarize the following contents: (1). The correlations and distributions of twin kHz QPOs; (2). The relations of high-low frequency QPOs; (3). The QPO properties of NS Atoll and Z sources; (4). No clear direct correlations between NS spins and QPOs; (5). The mechanisms of kHz QPOs; (6). The implications of kHZ QPOs, e.g., NS mass and radius, disk thickness and magnetic field of Atoll and Z source.

scholarly journals The Local Low-Mass Binary Pulsar Population

1996 ◽  
Vol 165 ◽  
pp. 235-241
Author(s):  
D.R. Lorimer
Keyword(s):  
Birth Rate ◽  
Galactic Plane ◽  
Space Velocity ◽  
Scale Height ◽  
Selection Effects ◽  
X Ray ◽  
Order Of Magnitude ◽  
Low Mass ◽  
The Mean ◽  
X Ray Binaries

Using a fully self-consistent approach to account for known survey selection effects, we constrain the number and scale height of low-mass binary pulsars (LMBPs) in the local solar neighbourhood. Our results show that the local surface density of LMBPs with luminosities above 2.5 mJy kpc2 is ∼20 kpc−2. Assuming that these are long-lived (≲1010 yr) objects, their local birth rate is at least 2 10−9 kpc−2 yr−1. Whilst this is in excellent agreement with the birth rate of their proposed progenitors, the low-mass X-ray binaries, there are several uncertainties involved which could significantly increase our derived birth rate, perhaps by an order of magnitude. Models in which the scale height of LMBPs above the galactic plane exceeds 500 pc are found to be most consistent with the data. The mean space velocity at birth required to produce scale heights of this order in 1010 yr is found to be ≳ 80 km s−1.

Iron K-Line Emission from X-Ray Binaries

1988 ◽  
Vol 102 ◽  
pp. 47-50
Author(s):  
K. Masai ◽  
S. Hayakawa ◽  
F. Nagase
Keyword(s):  
Accretion Disk ◽  
Radiative Recombination ◽  
Characteristic Temperature ◽  
Line Emission ◽  
Ionization Front ◽  
Continuum Radiation ◽  
X Ray ◽  
Low Mass ◽  
X Ray Binaries

AbstractEmission mechanisms of the iron Kα-lines in X-ray binaries are discussed in relation with the characteristic temperature Txof continuum radiation thereof. The 6.7 keV line is ascribed to radiative recombination followed by cascades in a corona of ∼ 100 eV formed above the accretion disk. This mechanism is attained for Tx≲ 10 keV as observed for low mass X-ray binaries. The 6.4 keV line observed for binary X-ray pulsars with Tx> 10 keV is likely due to fluorescence outside the He II ionization front.

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