scholarly journals Interpretations for Low‐ and High‐Frequency QPO Correlations of X‐Ray Sources among White Dwarfs, Neutron Stars, and Black Holes

2007 ◽  
Vol 119 (854) ◽  
pp. 393-397 ◽  
Author(s):  
C. M. Zhang ◽  
H. X. Yin ◽  
Y. H. Zhao
Keyword(s):  
Black Holes ◽  
Neutron Stars ◽  
High Frequency ◽  
White Dwarfs ◽  
X Ray

scholarly journals Non-Linear Resonances in Accretion Disks and QPOs

2004 ◽  
Vol 194 ◽  
pp. 128-129
Author(s):  
Włodek Kluźniak
Keyword(s):  
Black Holes ◽  
Neutron Stars ◽  
Accretion Disk ◽  
Accretion Disks ◽  
High Frequency ◽  
Light Curves ◽  
X Ray ◽  
Non Linear ◽  
Low Mass ◽  
X Ray Binaries

AbstractNon-linear oscillations in the accretion disk are favored as an explanation of high-frequency QPOs observed in the light curves of low-mass X-ray binaries containing neutron stars, black holes, or white dwarfs.

scholarly journals Multiwavelength Emission from Magnetically Arrested Disks around Isolated Black Holes

2021 ◽  
Vol 922 (1) ◽  
pp. L15
Author(s):  
Shigeo S. Kimura ◽  
Kazumi Kashiyama ◽  
Kenta Hotokezaka
Keyword(s):  
Black Holes ◽  
Synchrotron Radiation ◽  
Interstellar Medium ◽  
Neutron Stars ◽  
White Dwarfs ◽  
Gamma Ray ◽  
Optical Signals ◽  
X Ray ◽  
Nonthermal Electrons

Abstract We discuss the prospects for identifying the nearest isolated black holes (IBHs) in our Galaxy. IBHs accreting gas from the interstellar medium likely form magnetically arrested disks (MADs). We show that thermal electrons in the MADs emit optical signals through the thermal synchrotron process while nonthermal electrons accelerated via magnetic reconnections emit a flat-spectrum synchrotron radiation in the X-ray to MeV gamma-ray ranges. The Gaia catalog will include at most a thousand IBHs within ≲1 kpc that are distributed on and around the cooling sequence of white dwarfs (WDs) in the Hertzsprung–Russell diagram. These IBH candidates should also be detected by eROSITA, with which they can be distinguished from isolated WDs and neutron stars. Follow-up observations with hard X-ray and MeV gamma-ray satellites will be useful to unambiguously identify IBHs.

scholarly journals Halo/Thick Disk CVS and the Cosmic X-Ray Background

1996 ◽  
Vol 168 ◽  
pp. 543-548
Author(s):  
Jonathan E. Grindlay ◽  
Eyal Maoz
Keyword(s):  
Black Holes ◽  
Neutron Stars ◽  
Globular Clusters ◽  
White Dwarfs ◽  
Thick Disk ◽  
X Ray ◽  
Diffuse Flux ◽  
The Galaxy ◽  
X Ray Background

In a recent study (Maoz and Grindlay 1995) we have found that a number of previously recognized anomalies in the diffuse x-ray background at soft energies (~0.5-2 keV) can be understood if about 20-30% of the diffuse flux arises from a population of low luminosity sources in a thick disk or flattened halo distribution in the Galaxy. Here we summarize our results and review the arguements that these objects are not accreting neutron stars or black holes but rather white dwarfs (i.e. CVs) which may have been produced in a primordial population of disrupted globular clusters.

An efficient photoelectric X-ray polarimeter for the study of black holes and neutron stars

Nature ◽  
2001 ◽  
Vol 411 (6838) ◽  
pp. 662-665 ◽  
Author(s):  
Enrico Costa ◽  
Paolo Soffitta ◽  
Ronaldo Bellazzini ◽  
Alessandro Brez ◽  
Nicholas Lumb ◽  
...  
Keyword(s):  
Black Holes ◽  
Neutron Stars ◽  
X Ray

The stellar graveyard

2019 ◽  
pp. 177-206
Author(s):  
Nils Andersson
Keyword(s):  
Black Holes ◽  
General Relativity ◽  
Neutron Stars ◽  
Gravitational Wave ◽  
Stellar Evolution ◽  
White Dwarfs ◽  
Supermassive Black Holes ◽  
Compact Objects ◽  
Fermi Gases ◽  
The 1950S

This chapter introduces the different classes of compact objects—white dwarfs, neutron stars, and black holes—that are relevant for gravitational-wave astronomy. The ideas are placed in the context of developing an understanding of the likely endpoint(s) of stellar evolution. Key ideas like Fermi gases and the Chandrasekhar mass are discussed, as is the emergence of general relativity as a cornerstone of astrophysics in the 1950s. Issues associated with different formation channels for, in particular, black holes are considered. The chapter ends with a discussion of the supermassive black holes that are found at the centre of galaxies.

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