X-ray spectral analysis of the neutron star in SNR 1E 0102.2−7219

ABSTRACT We re-analysed numerous archival Chandra X-ray observations of the bright supernova remnant (SNR) 1E 0102.2−7219 in the Small Magellanic Cloud, to validate the detection of a neutron star (NS) in the SNR by Vogt et al. Careful attention to the background is necessary in this spectral analysis. We find that a blackbody + power-law model is a decent fit, suggestive of a relatively strong B field and synchrotron radiation, as in a normal young pulsar, though the thermal luminosity would be unusually high for young pulsars. Among realistic NS atmosphere models, a carbon atmosphere with B = 1012 G best fits the observed X-ray spectra. Comparing its unusually high thermal luminosity ($L_{\mathrm{ bol}} = 1.1_{-0.5}^{+1.6}\times 10^{34}$ erg s−1) to other NSs, we find that its luminosity can be explained by decay of an initially strong magnetic field (as in magnetars or high B-field pulsars) or by slower cooling after the supernova explosion. The nature of the NS in this SNR (and of others in the Magellanic Clouds) could be nicely confirmed by an X-ray telescope with angular resolution like Chandra, but superior spectral resolution and effective area, such as the Lynx concept.

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SALT observations of the supernova remnant MCSNR J0127−7332 and its associated Be X-ray binary SXP 1062 in the SMC

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/stab679 ◽

2021 ◽

Vol 503 (3) ◽

pp. 3856-3866

Author(s):

V V Gvaramadze ◽

A Y Kniazev ◽

J S Gallagher ◽

L M Oskinova ◽

Y-H Chu ◽

...

Keyword(s):

Neutron Star ◽

Emission Line ◽

Supernova Remnant ◽

Supernova Explosion ◽

High Mass ◽

Expansion Velocity ◽

X Ray ◽

Orbital Phase ◽

Be Star ◽

The Moment

ABSTRACT We report the results of optical spectroscopy of the Small Magellanic Cloud supernova remnant (SNR) MCSNR J0127−7332 and the mass donor Be star, 2dFS 3831, in its associated high-mass X-ray binary SXP 1062 carried out with the Southern African Large Telescope. Using high-resolution long-slit spectra, we measured the expansion velocity of the SNR shell of ${\approx} 140 \, {\rm \, km\, s^{-1}}$, indicating that MCSNR J0127−7332 is in the radiative phase. We found that the observed line ratios in the SNR spectrum can be understood if the local interstellar medium is ionized by 2dFS 3831 and/or OB stars around the SNR. We propose that MCSNR J0127−7332 is the result of supernova explosion within a bubble produced by the stellar wind of the supernova progenitor and that the bubble was surrounded by a massive shell at the moment of supernova explosion. We estimated the age of MCSNR J0127−7332 to be ${\lesssim} 10\, 000$ yr. We found that the spectrum of 2dFS 3831 changes with orbital phase. Namely, the equivalent width of the H α emission line decreased by ≈40 per cent in ≈130 d after periastron passage of the neutron star and then almost returned to its original value in the next ≈100 d. Also, the spectrum of 2dFS 3831 obtained closest to the periastron epoch (about 3 weeks after the periastron) shows a noticeable emission line of He ii λ4686, which disappeared in the next 2 weeks. We interpret these changes as a result of the temporary perturbation and heating of the disc as the neutron star passes through it.

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DO YOUNG NEUTRON STARS WHICH SHOW THEMSELVES AS AXPs AND SGRs ACCRETE?

International Journal of Modern Physics D ◽

10.1142/s0218271803003438 ◽

2003 ◽

Vol 12 (05) ◽

pp. 825-831 ◽

Cited By ~ 3

Author(s):

S. O. TAGIEVA ◽

E. YAZGAN ◽

A. ANKAY

Keyword(s):

Neutron Star ◽

Neutron Stars ◽

Supernova Explosion ◽

X Ray ◽

X Ray Binaries

We examined the fall-back disk models, and in general accretion, proposed to explain the properties of AXPs and SGRs. We checked the possibility of some gas remaining around the neutron star after a supernova explosion. We also compared AXPs and SGRs with the X-ray pulsars in X-ray binaries. We conclude that the existing models of accretion from a fall-back disk are insufficient to explain the nature of AXPs and SGRs.

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Supernova Remnant Searches at Molonglo

Publications of the Astronomical Society of Australia ◽

10.1017/s1323358000017549 ◽

1984 ◽

Vol 5 (4) ◽

pp. 537-540 ◽

Cited By ~ 9

Author(s):

A. J. Turtle ◽

B. Y. Mills

Keyword(s):

Supernova Remnants ◽

Supernova Remnant ◽

Magellanic Clouds ◽

Radio Observations ◽

X Ray

A catalogue of 38 supernova remnants (SNRs) identified in the Large and Small Magellanic Clouds from X-ray, optical and radio observations has recently been presented by Mills et al. (1984). One important consideration is the completeness of this catalogue and of the Galactic catalogues with which it is compared. These are currently being investigated.

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The Gamma-ray Large Area Space Telescope (GLAST)

International Astronomical Union Colloquium ◽

10.1017/s0252921100001251 ◽

2002 ◽

Vol 187 ◽

pp. 73-77

Author(s):

Taro Kotani

Keyword(s):

International Collaboration ◽

Gamma Ray ◽

Angular Resolution ◽

Effective Area ◽

Low Earth Orbit ◽

Gamma Ray Bursts ◽

Earth Orbit ◽

Large Area ◽

X Ray ◽

Primary Instrument

AbstractGLAST, the next U.S. general gamma-ray astrophysics mission scheduled to be launched into low Earth orbit in April, 2006, for 5–10 years of operation, is described. A product of a NASA/DOE and international collaboration, the Large Area Telescope (LAT) is the primary instrument that covers the < 20 MeV to > 300 GeV band with an effective area > 8000 cm2. The angular resolution ranges from < 3.5° at 100 MeV to < 0.15° at 10 GeV. The GLAST Burst Monitor (GBM) consists of a group of NaI and BGO detectors to extend GLAST’s sensitivity to gamma-ray bursts to the < 10 keV to > 25 MeV band. GLAST’s localizations enables us to identify the X-ray, optical and radio counterparts of thousands of gamma-ray sources and to determine their nature.

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Intensive X-ray Monitoring of the 16ms Crab-like Pulsar PSR J0537 – 6910

International Astronomical Union Colloquium ◽

10.1017/s0252921100059911 ◽

2000 ◽

Vol 177 ◽

pp. 335-340

Author(s):

F. E. Marshall ◽

E. V. Gotthelf ◽

J. Middleditch ◽

Q. D. Wang ◽

W. Zhang

Keyword(s):

Neutron Star ◽

Maximum Rate ◽

Supernova Remnant ◽

Large Magellanic Cloud ◽

Crab Pulsar ◽

Pulsar Emission ◽

X Ray ◽

Intensive Monitoring ◽

Unique Probe ◽

Pulse Timing

AbstractThe recently discovered pulsar PSR J0537-6910 is the most rapidly rotating young pulsar known. This latest example of a Crab-like pulsar, located in the supernova remnant N157B in the Large Magellanic Cloud, is rotating twice as fast as the Crab pulsar. With a characteristic age of 5000 years, it is also the oldest known example of a Crab-like pulsar and was likely rotating close to the maximum rate for a neutron star when it was born. Here we report preliminary results from an intensive monitoring campaign of X-ray observations acquired with the Rossi X-ray Timing Explorer that began in January 1999. These observation have revealed a large glitch event in the pulse timing during the first six month of our campaign, consistent with those suggested by sparse observations dating back to 1993. The current evolution of the rotation rate of PSR J0537-6910 provides a unique probe of the internal structure of neutron stars and constraints on possible pulsar emission mechanisms.

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NuSTAR observations of rotation-powered pulsars and magnetars

Proceedings of the International Astronomical Union ◽

10.1017/s1743921312024027 ◽

2012 ◽

Vol 8 (S291) ◽

pp. 331-336

Author(s):

V. M. Kaspi ◽

H. An ◽

M. Bachetti ◽

E. Bellm ◽

A. M. Beloborodov ◽

...

Keyword(s):

Point Source ◽

Angular Resolution ◽

Focal Length ◽

Effective Area ◽

X Ray ◽

Large Effective Area ◽

Better Than

AbstractNASA's NuSTAR observatory is the first focusing hard X-ray telescope. Launched in June 2012, NuSTAR is sensitive in the 3–79 keV range with unprecedented ~17″ FWHM angular resolution above 12 keV, a result of its multilayer-coated optics and 10-m focal length. With its large effective area (900 cm2 at 10 keV), NuSTAR has point-source sensitivity ~100 times better than previous hard X-ray telescopes. Here we describe NuSTAR and its planned work on rotation-powered pulsars and magnetars during its nominal 2-yr baseline mission that has just commenced.

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PULSAR KICKS AND DARK MATTER FROM A STERILE NEUTRINO

International Journal of Modern Physics A ◽

10.1142/s0217751x0502402x ◽

2005 ◽

Vol 20 (06) ◽

pp. 1148-1154 ◽

Cited By ~ 1

Author(s):

ALEXANDER KUSENKO

Keyword(s):

Dark Matter ◽

Neutron Star ◽

Gravitational Wave ◽

Sterile Neutrino ◽

Supernova Explosion ◽

Radio Pulsars ◽

X Ray ◽

Gravitational Wave Detectors ◽

Rule Out

The observed velocities of radio pulsars, which range in the hundreds kilometers per second, and many of which exceed 1000 km/s, are not explained by the standard physics of the supernova explosion. However, if a sterile neutrino with mass in the 1–20 keV range exists, it would be emitted asymmetrically from a cooling neutron star, which could give it a sufficient recoil to explain the pulsar motions. The same particle can be the cosmological dark mater. Future observations of X-ray telescopes and gravitational wave detectors can confirm or rule out this explanation.

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Evidence from high-mass X-ray binaries that Galactic WR components of WR+O binaries end their life with a supernova explosion

Astronomy and Astrophysics ◽

10.1051/0004-6361/201937253 ◽

2020 ◽

Vol 636 ◽

pp. A99 ◽

Cited By ~ 3

Author(s):

D. Vanbeveren ◽

N. Mennekens ◽

E. P. J. van den Heuvel ◽

J. Van Bever

Keyword(s):

Black Hole ◽

Neutron Star ◽

Supernova Explosion ◽

Solar Neighborhood ◽

High Mass ◽

Population Number ◽

X Ray ◽

Theoretical Population ◽

X Ray Binaries

Context. Theoretical population number studies of binaries with at least one black hole (BH) component obviously depend on whether or not BHs receive a (natal) kick during their formation. Aims. Several observational facts seem to indicate that BHs do indeed receive a kick during their formation. In the present paper, we discuss additional evidence of this. Methods. The progenitors of wind-fed high-mass X-ray binaries (HMXB) with a BH component (BH HMXB) are WR+OB binaries where the Wolf–Rayet (WR) star will finally collapse and form the BH. Starting from the observed population of WR+OB binaries in the solar neighborhood, we predict the population of wind-fed BH HMXBs as a function of the BH-natal kick. Results. The simulations reveal that when WR stars collapse into a BH with a zero or low kick, we should expect 100 or more wind-fed BH HMXBs in the solar neighborhood, whereas only one is observed (Cyg X-1). We consider this as evidence that either WR components in binaries end their life as a neutron star or that they collapse into BHs, both accompanied by a supernova explosion imparting significant (natal) kicks.

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Be/X-Ray Binaries with Black Holes in the Galaxy and in the Magellanic Clouds

Acta Polytechnica CTU Proceedings ◽

10.14311/app.2014.01.0175 ◽

2014 ◽

Vol 1 (1) ◽

pp. 175-180 ◽

Cited By ~ 3

Author(s):

Janusz Ziolkowski

Keyword(s):

Black Holes ◽

Black Hole ◽

Neutron Star ◽

Magellanic Clouds ◽

X Ray ◽

The Galaxy ◽

X Ray Binaries ◽

Successful Candidate

I will start with the statistics indicating that the objects named in the title of my talk are either non-existing or very elusive to detect (not a single such object is known against 119 known Be/neutron star X-ray binaries). After brief reviewing of the properties of Be/X-ray binaries I discuss several objects that were proposed as the long sought for candidates for Be/black hole X-ray binaries. After three unsuccessful candidates (LS I +61° 303, LS 5039 and MAXI J1836-194), a successful candidate (AGL J2241+4454/MWC 656) was finally, very recently, announced.

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