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

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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Pulse Timing and Neutron Star Structure

Symposium - International Astronomical Union ◽

10.1017/s0074180900093037 ◽

1981 ◽

Vol 95 ◽

pp. 279-290

Author(s):

Paul E. Boynton

Keyword(s):

Neutron Star ◽

Timing Analysis ◽

Crab Pulsar ◽

X Ray ◽

Pulse Timing ◽

Star Structure

The implementation of pulse timing analysis as a probe of neutron star structure is reviewed for both pulsars and X-ray pulsators. Current results are particularly significant for the Crab pulsar.

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Superfluidity in Neutron Stars

Symposium - International Astronomical Union ◽

10.1017/s0074180900099988 ◽

1974 ◽

Vol 53 ◽

pp. 151-165

Author(s):

George Greenstein

Keyword(s):

Neutron Star ◽

Neutron Stars ◽

Crab Nebula ◽

Crab Pulsar ◽

X Ray ◽

Effects Of Rotation ◽

The Crab Nebula

We present a short Cook's tour of the possible effects of rotation coupled with superfluid properties of neutron star interiors. A suggestion is made to take advantage of forthcoming lunar occultations of the Crab Nebula in order to search for blackbody X-ray emission from the Crab pulsar.

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Enhanced x-ray emission coinciding with giant radio pulses from the Crab Pulsar

Science ◽

10.1126/science.abd4659 ◽

2021 ◽

Vol 372 (6538) ◽

pp. 187-190

Author(s):

Teruaki Enoto ◽

Toshio Terasawa ◽

Shota Kisaka ◽

Chin-Ping Hu ◽

Sebastien Guillot ◽

...

Keyword(s):

Optical Emission ◽

Crab Pulsar ◽

Radio Bursts ◽

Emission Mechanism ◽

Pulsar Emission ◽

X Ray ◽

Percentage Points

Giant radio pulses (GRPs) are sporadic bursts emitted by some pulsars that last a few microseconds and are hundreds to thousands of times brighter than regular pulses from these sources. The only GRP-associated emission outside of radio wavelengths is from the Crab Pulsar, where optical emission is enhanced by a few percentage points during GRPs. We observed the Crab Pulsar simultaneously at x-ray and radio wavelengths, finding enhancement of the x-ray emission by 3.8 ± 0.7% (a 5.4σ detection) coinciding with GRPs. This implies that the total emitted energy from GRPs is tens to hundreds of times higher than previously known. We discuss the implications for the pulsar emission mechanism and extragalactic fast radio bursts.

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N49: The Site of a Gamma-ray Burst. Preliminary Results from X-ray Observations

Symposium - International Astronomical Union ◽

10.1017/s0074180900034458 ◽

1983 ◽

Vol 101 ◽

pp. 573-577

Author(s):

G. Pizzichini ◽

T. L. Cline ◽

U. D. Desai ◽

B. J. Teegarden ◽

W. D. Evans ◽

...

Keyword(s):

High Resolution ◽

Supernova Remnant ◽

Gamma Ray ◽

Large Magellanic Cloud ◽

X Rays ◽

Radio Image ◽

Gamma Ray Burst ◽

X Ray ◽

Preliminary Results ◽

Einstein Observatory

The error box of the unusual Gamma-Ray Burst of March 5, 1979 falls completely inside the optical and radio image of the Supernova Remnant N49 in the Large Magellanic Cloud. This region was observed twice in x-rays with the High Resolution Imager of the Einstein Observatory, six weeks and nearly two years after the Gamma-Ray Burst. We show the comparison between the two observations.

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Probing X-ray emission in different modes of PSR J1023+0038 with a radio pulsar scenario

Astronomy and Astrophysics ◽

10.1051/0004-6361/201936312 ◽

2019 ◽

Vol 629 ◽

pp. L8 ◽

Cited By ~ 3

Author(s):

S. Campana ◽

A. Miraval Zanon ◽

F. Coti Zelati ◽

D. F. Torres ◽

M. C. Baglio ◽

...

Keyword(s):

Neutron Star ◽

Spectral Properties ◽

Source Parameters ◽

High Mode ◽

Radio Pulsar ◽

Emission Model ◽

Emission Mechanism ◽

Pulsar Emission ◽

X Ray ◽

Pulsar Wind

Transitional pulsars provide us with a unique laboratory to study the physics of accretion onto a magnetic neutron star. PSR J1023+0038 (J1023) is the best studied of this class. We investigate the X-ray spectral properties of J1023 in the framework of a working radio pulsar during the active state. We modelled the X-ray spectra in three modes (low, high, and flare) as well as in quiescence, to constrain the emission mechanism and source parameters. The emission model, formed by an assumed pulsar emission (thermal and magnetospheric) plus a shock component, can account for the data only adding a hot dense absorber covering ∼30% of the emitting source in high mode. The covering fraction is similar in flaring mode, thus excluding total enshrouding, and decreases in the low mode despite large uncertainties. This provides support to the recently advanced idea of a mini-pulsar wind nebula (PWN), where X-ray and optical pulsations arise via synchrotron shock emission in a very close (∼100 km, comparable to a light cylinder), PWN-like region that is associated with this hot absorber. In low mode, this region may expand, pulsations become undetectable, and the covering fraction decreases.

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RX J050736−6847.8: A Large Supernova Remnant around an X-Ray Binary in the Large Magellanic Cloud

The Astronomical Journal ◽

10.1086/301331 ◽

2000 ◽

Vol 119 (5) ◽

pp. 2242-2247 ◽

Cited By ~ 13

Author(s):

You-Hua Chu ◽

Sungeun Kim ◽

Sean D. Points ◽

Robert Petre ◽

Steven L. Snowden

Keyword(s):

Supernova Remnant ◽

Large Magellanic Cloud ◽

Magellanic Cloud ◽

X Ray

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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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POSSIBLE SIGNATURES OF THE CONVERSION OF A NEUTRON STAR TO A STRANGE STAR

International Journal of Modern Physics D ◽

10.1142/s0218271894000794 ◽

1994 ◽

Vol 03 (03) ◽

pp. 653-664

Author(s):

O.G. BENVENUTO ◽

M.I. KRIVORUCHENKO ◽

B.V. MARTEMYANOV

Keyword(s):

Neutron Star ◽

Neutron Stars ◽

High Recurrence Rate ◽

Massive Quark ◽

Pulsar Emission ◽

Strange Stars ◽

X Ray ◽

Supernova Explosions ◽

Low Mass ◽

Step Mechanism

The problem of the identification of strange stars is discussed. We suggest some characteristic signatures for the search for strange stars: a two-step mechanism for supernova explosions accompanied by the occurrence of strange stars and two neutrino bursts; microstructure analysis in the profile of pulsar emission; and unusual stability in the rotation of millisecond pulsars due to the absence of internal crust in strange stars. The cooling of strange stars is faster than the cooling of ordinary neutron stars, so low surface temperature of pulsars can indicate the existence of massive quark cores in observed pulsars. Low mass strange stars as bursters and/or X-ray sources have peculiar observable features: low luminosity and (for bursters) high recurrence rate, large duration of bursts, low ratio of energy emitted between two bursts and energy emitted during the burst.

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Observations of G320.4–1.2 and Speculations on Supernova Remnant Morphology

Symposium - International Astronomical Union ◽

10.1017/s0074180900034227 ◽

1983 ◽

Vol 101 ◽

pp. 421-427

Author(s):

R. N. Manchester ◽

J. M. Durdin

Keyword(s):

Binary System ◽

Supernova Remnant ◽

Rotational Energy ◽

Crab Pulsar ◽

X Ray ◽

North West ◽

The North ◽

Pulsar Timing ◽

Period Derivative ◽

Galactic Radio

The galactic radio source G320.4–1.2 (MSH15–52) consists of several components, the most prominent of which is situated in the north-west quadrant and is associated with the Hα nebula RCW89. Caswell et al. (1981) mapped the source at 1.4 GHz with a resolution of 50″ arc and concluded that it was a single supernova remnant with all components having spectral index α ≈ −0.34. This SNR has become more significant with the recent discovery (Seward and Harnden, 1982) of an X-ray pulsar of period 150 ms at the position (1950) R.A. 15h09m59s.5, Dec. −58°56′57″ near the centre of the remnant and the detection of this pulsar at radio frequencies (Manchester et al., 1982). The pulsar has some similarities to the Crab pulsar in that its period derivative is extremely high and hence its characteristic age low, ∼1570 years, comparable to that of the Crab pulsar. Timing observations (Manchester and Durdin, unpublished) indicate that the pulsar is not a member of a binary system and hence that the pulsed X-ray emission is powered by rotational energy, as in the Crab pulsar.

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