scholarly journals Sizing Up the Most Massive Neutron Star

Physics ◽  
2021 ◽  
Vol 14 ◽  
Author(s):  
Matteo Rini
Keyword(s):  
Neutron Star ◽  
Massive Neutron Star

scholarly journals A New Likely Redback Millisecond Pulsar Binary with a Massive Neutron Star: 4FGL J2333.1–5527

2020 ◽  
Vol 892 (1) ◽  
pp. 21 ◽  
Author(s):  
Samuel J. Swihart ◽  
Jay Strader ◽  
Ryan Urquhart ◽  
Jerome A. Orosz ◽  
Laura Shishkovsky ◽  
...  
Keyword(s):  
Neutron Star ◽  
Millisecond Pulsar ◽  
Massive Neutron Star

scholarly journals Probing the stellar wind geometry in Vela X-1 with infrared interferometry

2012 ◽  
Vol 8 (S290) ◽  
pp. 197-198
Author(s):  
Élodie Choquet ◽  
Pierre Kervella ◽  
Jean-Baptiste Le Bouquin ◽  
Antoine Mérand ◽  
Xavier Haubois ◽  
...  
Keyword(s):  
Neutron Star ◽  
High Mass ◽  
Resolution Limit ◽  
X Ray ◽  
Upper Limit ◽  
Accretion Process ◽  
Massive Neutron Star ◽  
Infrared Interferometry ◽  
X Ray Binaries ◽  
K Band

AbstractHigh-mass X-ray Binaries (HMXBs) are keys to study stellar remnants that are otherwise extremely faint and difficult to observe when isolated. Vela X-1 is a well-known eclipsing HMXB composed of a very massive neutron star orbiting a B0.5I supergiant with a period of 9 days. The supergiant wind is the main feeding material for the accreting neutron star, and its properties are of prime interest to understand the physics at stakes in the accretion process.In order to characterize the geometry and physical properties of the dense wind at a scale of a few stellar radii, we obtained infrared interferometric observations of Vela X-1 in 2010 using the VLTI/AMBER instrument in the K band (2.2 μm), and in 2012 using the VLTI/PIONIER instrument in the H band (1.6 μm).Although the apparent disk of the supergiant and the orbital separation of the two objects are beyond the present resolution limit of the VLTI, the K-band observations partially resolve the wind envelope on the two longest baselines. We were able to measure the radius of 265±82 R⊙ for the circumstellar wind at a temperature of 1300 K, assuming a distance of 1.9 kpc. The H-band observations do not resolve the system, and we were able to set an upper limit of 112 R⊙ for the envelope radius at a temperature of 1800 K.

scholarly journals 1FGL J1417.7–4407: A LIKELY GAMMA-RAY BRIGHT BINARY WITH A MASSIVE NEUTRON STAR AND A GIANT SECONDARY

2015 ◽  
Vol 804 (1) ◽  
pp. L12 ◽  
Author(s):  
Jay Strader ◽  
Laura Chomiuk ◽  
C. C. Cheung ◽  
David J. Sand ◽  
Davide Donato ◽  
...  
Keyword(s):  
Neutron Star ◽  
Gamma Ray ◽  
Massive Neutron Star

scholarly journals Collimated outflows from long-lived binary neutron star merger remnants

2020 ◽  
Vol 495 (1) ◽  
pp. L66-L70 ◽  
Author(s):  
Riccardo Ciolfi
Keyword(s):  
Black Hole ◽  
Neutron Star ◽  
Gamma Ray ◽  
Gamma Ray Bursts ◽  
Spin Axis ◽  
Binary Neutron Star ◽  
Physical Conditions ◽  
Massive Neutron Star ◽  
Merger Event ◽  
First Time

ABSTRACT The connection between short gamma-ray bursts (SGRBs) and binary neutron star (BNS) mergers was recently confirmed by the association of GRB 170817A with the merger event GW170817. However, no conclusive indications were obtained on whether the merger remnant that powered the SGRB jet was an accreting black hole (BH) or a long-lived massive neutron star (NS). Here, we explore the latter case via BNS merger simulations covering up to 250 ms after merger. We report, for the first time in a full merger simulation, the formation of a magnetically driven collimated outflow along the spin axis of the NS remnant. For the system at hand, the properties of such an outflow are found largely incompatible with an SGRB jet. With due consideration of the limitations and caveats of our present investigation, our results favour a BH origin for GRB 170817A and SGRBs in general. Even though this conclusion needs to be confirmed by exploring a larger variety of physical conditions, we briefly discuss possible consequences of all SGRB jets being powered by accreting BHs.

scholarly journals Binary evolution leading to the formation of the very massive neutron star in the J0740+6620 binary system

2020 ◽  
Vol 495 (2) ◽  
pp. 2509-2514
Author(s):  
M Echeveste ◽  
M L Novarino ◽  
O G Benvenuto ◽  
M A De Vito
Keyword(s):  
Neutron Star ◽  
Binary System ◽  
Effective Temperature ◽  
Binary Systems ◽  
Close Binary ◽  
Normal Donor ◽  
Millisecond Pulsar ◽  
Massive Neutron Star ◽  
Binary Evolution ◽  
Age Of The Universe

ABSTRACT We study the evolution of close binary systems in order to account for the existence of the recently observed binary system containing the most massive millisecond pulsar ever detected, PSR J0740+6620, and its ultra-cool helium white dwarf companion. In order to find a progenitor for this object we compute the evolution of several binary systems composed by a neutron star and a normal donor star employing our stellar code. We assume conservative mass transfer. We also explore the effects of irradiation feedback on the system. We find that irradiated models also provide adequate models for the millisecond pulsar and its companion, so both irradiated and non irradiated systems are good progenitors for PSR J0740+6620. Finally, we obtain a binary system that evolves and accounts for the observational data of the system composed by PSR J0740+6620 (i.e. orbital period, mass, effective temperature and inferred metallicity of the companion, and mass of the neutron star) in a time scale smaller than the age of the Universe. In order to reach an effective temperature as low as observed, the donor star should have an helium envelope as demanded by observations.

scholarly journals The Massive Neutron Star or Low-Mass Black Hole in 2S 0921-630

2004 ◽  
Vol 616 (2) ◽  
pp. L123-L126 ◽  
Author(s):  
T. Shahbaz ◽  
J. Casares ◽  
C. A. Watson ◽  
P. A. Charles ◽  
R. I. Hynes ◽  
...  
Keyword(s):  
Black Hole ◽  
Neutron Star ◽  
Massive Neutron Star ◽  
Low Mass
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