Results 71 to 80 of about 910,791 (369)
SUPERFLUID NEUTRON STARS [PDF]
The Ninth Marcel Grossmann Meeting, 2002 2 pages, "mprocl.sty" with LaTeX 2.09; contribution to the 9th Marcel Grossmann Meeting (MG9), Rome, July ...
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Sonoluminescence in neutron stars [PDF]
Physics Letters B, 1998 After a brief discussion of a possible relationship between the electroweak phase transition in highly compressed matter and gravitational collapse, we examine the speculative possibility that the electroweak phase transition might be contemporarily occurring in processes in neutron stars. We conjecture that adiabatic compression of neutron star matter
John G. Learned +3 more
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A Chandra observation of the long-duration X-ray transient KS 1731-260 in quiescence: too cold a neutron star? [PDF]
, 2001 After more than a decade of actively accreting at about a tenth of the Eddington critical mass accretion rate, the neutron-star X-ray transient KS 1731-260 returned to quiescence in early 2001. We present a Chandra/ACIS-S observation taken several months
Asai K. +12 more
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The Possibility of the Secondary Object in GW190814 as a Neutron Star [PDF]
Astrophysical Journal, 2020 A compact object was observed with a mass of by LIGO Scientific and Virgo collaborations (LVC) in GW190814, which provides a great challenge to investigations of supranuclear matter.
Kaixuan Huang +3 more
semanticscholar +1 more source
The Zoo of neutron stars [PDF]
Physics of Particles and Nuclei, 2008 In these lecture notes I briefly discuss the present day situation and new discoveries in astrophysics of neutron stars focusing on isolated objects. The latter include soft gamma repeaters, anomalous X-ray pulsars, central compact objects in supernova remnants, the Magnificent seven, and rotating radio transients.
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Physica Scripta, 2000 15 pages, LaTeX2e, 3 eps figures, to appear in Physica ...
Ilona Bednarek, Ryszard Manka
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Bayesian Model Selection of Unified Neutron Star EOSs in Multi-messenger Era
Yuanzineng kexue jishu, 2023 The equation of state (EoS) of neutron star matter plays a key role in both the structure and evolution of a neutron star. However, as lattice QCD faces significant difficulties in simulating dense matter, only effective models can be relied on to unveil
RUI Xingyu;MIAO Zhiqiang;XIA Chengjun
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Time Evolution of Relativistic Force-Free Fields Connecting a Neutron Star and its Disk
, 2005 We study the magnetic interaction between a neutron star and its disk by solving the time-dependent relativistic force-free equations. At the initial state, we assume that the dipole magnetic field of the neutron star connects the neutron star and its ...
Asano, Eiji +2 more
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Neutron skins and neutron stars
Physical Review C, 2012 Background: The neutron skin of a heavy nucleus as well as many neutron-star properties are highly sensitive to the poorly constrained density dependence of the symmetry energy. Purpose: To provide for the first time meaningful theoretical errors and to assess the degree of correlation between the neutron-skin thickness of ${}^{208}$Pb and several ...
Farrukh J. Fattoyev +2 more
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A magnetically driven origin for the low luminosity GRB 170817A associated with GW170817
, 2018 The gamma-ray burst GRB 170817A associated with GW170817 is subluminous and subenergetic compared with other typical short GRBs. It may be due to a relativistic jet viewed off-axis, or a structured jet, or cocoon emission. Giant flares from magnetars may
Huang, L., Tong, H., Yu, C.
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