scholarly journals Designing a cross-correlation search for continuous-wave gravitational radiation from a neutron star in the supernova remnant SNR 1987A★

2011 ◽  
Vol 414 (3) ◽  
pp. 2650-2663 ◽  
Author(s):  
C. T. Y. Chung ◽  
A. Melatos ◽  
B. Krishnan ◽  
J. T. Whelan
Keyword(s):  
Neutron Star ◽  
Gravitational Radiation ◽  
Supernova Remnant ◽  
Cross Correlation ◽  
Continuous Wave ◽  
Correlation Search

scholarly journals Modelling neutron star mountains

2020 ◽  
Vol 500 (4) ◽  
pp. 5570-5582
Author(s):  
F Gittins ◽  
N Andersson ◽  
D I Jones
Keyword(s):  
Neutron Star ◽  
Neutron Stars ◽  
Gravitational Radiation ◽  
Continuous Wave ◽  
Pressure Perturbation ◽  
Will Emit ◽  
Thermal Pressure ◽  
The Core ◽  
Neutron Star Crust ◽  
Crucial Ingredient

ABSTRACT As the era of gravitational-wave astronomy has well and truly begun, gravitational radiation from rotating neutron stars remains elusive. Rapidly spinning neutron stars are the main targets for continuous-wave searches since, according to general relativity, provided they are asymmetrically deformed, they will emit gravitational waves. It is believed that detecting such radiation will unlock the answer to why no pulsars have been observed to spin close to the break-up frequency. We review existing studies on the maximum mountain that a neutron star crust can support, critique the key assumptions and identify issues relating to boundary conditions that need to be resolved. In light of this discussion, we present a new scheme for modelling neutron star mountains. The crucial ingredient for this scheme is a description of the fiducial force which takes the star away from sphericity. We consider three examples: a source potential which is a solution to Laplace’s equation, another solution which does not act in the core of the star and a thermal pressure perturbation. For all the cases, we find that the largest quadrupoles are between a factor of a few to two orders of magnitude below previous estimates of the maximum-mountain size.

scholarly journals Detection and Localization for Multiple Stationary Human Targets Based on Cross-Correlation of Dual-Station SFCW Radars

2019 ◽  
Vol 11 (12) ◽  
pp. 1428 ◽  
Author(s):  
Yong Jia ◽  
Yong Guo ◽  
Chao Yan ◽  
Haoxuan Sheng ◽  
Guolong Cui ◽  
...  
Keyword(s):  
Cross Correlation ◽  
Continuous Wave ◽  
Coefficient Matrix ◽  
Constant False Alarm Rate ◽  
Localization Algorithm ◽  
Cfar Detection ◽  
Stepped Frequency ◽  
The Cross ◽  
The One ◽  
Detection And Localization

This paper demonstrates the feasibility of detection and localization of multiple stationary human targets based on cross-correlation of the dual-station stepped-frequency continuous-wave (SFCW) radars. Firstly, a cross-correlation operation is performed on the preprocessed pulse signals of two SFCW radars at different locations to obtain the correlation coefficient matrix. Then, the constant false alarm rate (CFAR) detection is applied to extract the ranges between each target and the two radars, respectively, from the correlation matrix. Finally, the locations of human targets is calculated with the triangulation localization algorithm. This cross-correlation operation mainly brings about two advantages. On the one hand, the cross-correlation explores the correlation feature of target respiratory signals, which can effectively detect all targets with different signal intensities, avoiding the missed detection of weak targets. On the other hand, the pairing of two ranges between each target and two radars is implemented simultaneously with the cross-correlation. Experimental results verify the effectiveness of this algorithm.

scholarly journals A neutron star with a carbon atmosphere in the Cassiopeia A supernova remnant

Nature ◽  
2009 ◽  
Vol 462 (7269) ◽  
pp. 71-73 ◽  
Author(s):  
Wynn C. G. Ho ◽  
Craig O. Heinke
Keyword(s):  
Neutron Star ◽  
Supernova Remnant ◽  
Cassiopeia A

scholarly journals Probe position correction based on overlapped object wavefront cross-correlation for continuous-wave terahertz ptychography

2019 ◽  
Vol 27 (2) ◽  
pp. 938 ◽  
Author(s):  
Lu Rong ◽  
Chao Tang ◽  
Dayong Wang ◽  
Bing Li ◽  
Fangrui Tan ◽  
...  
Keyword(s):  
Cross Correlation ◽  
Continuous Wave ◽  
Probe Position ◽  
Position Correction

scholarly journals Gamma-Ray Bursts and Binary Neutron Star Mergers

1996 ◽  
Vol 165 ◽  
pp. 489-502
Author(s):  
Tsvi Piran
Keyword(s):  
Neutron Star ◽  
Gravitational Radiation ◽  
Gamma Ray ◽  
Indirect Evidence ◽  
Gamma Ray Bursts ◽  
Binary Neutron Star ◽  
Merger Event ◽  
Γ Rays ◽  
Γ Ray ◽  
The One

Neutron star binaries, such as the one observed in the famous binary pulsar PSR 1913+16, end their life in a catastrophic merger event (denoted here NS2M). The merger releases ∼5 1053 ergs, mostly as neutrinos and gravitational radiation. A small fraction of this energy suffices to power γ-ray bursts (GRBs) at cosmological distances. Cosmological GRBs must pass, however, an optically thick fireball phase and the observed γ rays emerge only at the end of this phase. Hence, it is difficult to determine the nature of the source from present observations (the agreement between the rates of GRBs and NS2Ms providing only indirect evidence for this model). In the future a coinciding detection of a GRB and a gravitational-radiation signal could confirm this model.

scholarly journals Continuous-wave gravitational radiation from pulsar glitch recovery

2010 ◽  
Vol 409 (4) ◽  
pp. 1705-1718 ◽  
Author(s):  
M. F. Bennett ◽  
C. A. Van Eysden ◽  
A. Melatos
Keyword(s):  
Gravitational Radiation ◽  
Continuous Wave

scholarly journals Chandra Study of the Central Object Associated with the Supernova Remnant MSH 11–62

2004 ◽  
Vol 218 ◽  
pp. 203-206
Author(s):  
Ilana Harrus ◽  
Joseph P. Bernstein ◽  
Patrick O. Slane ◽  
Bryan Gaensler ◽  
John P. Hughes ◽  
...  
Keyword(s):  
Neutron Star ◽  
Radio Emission ◽  
Supernova Remnant ◽  
Loss Rate ◽  
Thermal Emission ◽  
Compact Object ◽  
Small Region ◽  
Compact Source ◽  
Synchrotron Nebula ◽  
Compact Array

We present results from our analysis of Chandra data on the supernova remnant MSH 11–62 (also known as G291.0−0.1). Our previous ASCA analysis showed that MSH 11–62 is most likely a composite remnant whose strong non-thermal emission is powered by a compact object, most probably a pulsar. The present analysis confirms in a spectacular fashion the earlier detection of a compact source. The Chandra data reveal a small region with a hard non-thermal spectrum located at the tip of the central radio emission seen in data taken at the Australia Telescope Compact Array (ATCA). This source is likely the young rapidly rotating neutron star powering the synchrotron nebula in MSH 11–62. Compared to other young rotation-powered pulsars the Chandra specrum of MSH 11–62 implies an energy loss rate of Ė ∼ 5 × 1036 ergs s−1.

The properties of the progenitor, neutron star, and pulsar wind in the supernova remnant Kes 75

2014 ◽  
Vol 335 (3) ◽  
pp. 318-323 ◽  
Author(s):  
J. D. Gelfand ◽  
P. O. Slane ◽  
T. Temim
Keyword(s):  
Neutron Star ◽  
Supernova Remnant ◽  
Pulsar Wind

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

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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