Measurement of neutron star parameters: A review of methods for low-mass X-ray binaries

Bhattacharyya, Sudip

doi:10.1016/j.asr.2010.01.010

Cited by 68 publications

(97 citation statements)

References 245 publications

(260 reference statements)

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“…Spectral and timing properties of non-accreting millisecond radio pulsars can also be useful to measure stellar mass and radius (e.g., ;Bogdanov et al (2008)). However, until recently theoretically proposed EoS models could not be effectively constrained because of systematic uncertainties (e.g., Bhattacharyya (2010)). …”

Section: Introductionmentioning

confidence: 99%

“…Determining the correct EoS model describing the interior of compact stars is a funda-⋆ E-mail: sudip@tifr.res.in mental problem of physics, and a major effort has been made during the last few decades to solve this problem by measuring the stellar bulk properties. A number of these measurement methods for low-mass X-ray binaries (LMXBs), based on thermonuclear X-ray bursts, regular X-ray pulsations, high-frequency quasi-periodic oscillations, broad relativistic spectral emission lines, quiescent emissions and orbital motions, have been reviewed in Bhattacharyya (2010). Spectral and timing properties of non-accreting millisecond radio pulsars can also be useful to measure stellar mass and radius (e.g., ;Bogdanov et al (2008)).…”

Section: Introductionmentioning

confidence: 99%

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Fast spinning strange stars: possible ways to constrain interacting quark matter parameters

Bhattacharyya

Bombaci

Logoteta

et al. 2016

Mon. Not. R. Astron. Soc.

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For a set of equation of state (EoS) models involving interacting strange quark matter, characterized by an effective bag constant (B eff ) and a perturbative QCD corrections term (a 4 ), we construct fully general relativistic equilibrium sequences of rapidly spinning strange stars for the first time. Computation of such sequences is important to study millisecond pulsars and other fast spinning compact stars. Our EoS models can support a gravitational mass (M G ) and a spin frequency (ν) at least up to ≈ 3.0M ⊙ and ≈ 1250 Hz respectively, and hence are fully consistent with measured M G and ν values. This paper reports the effects of B eff and a 4 on measurable compact star properties, which could be useful to find possible ways to constrain these fundamental quark matter parameters, within the ambit of our EoS models. We confirm that a lower B eff allows a higher mass. Besides, for known M G and ν, measurable parameters, such as stellar radius, radius-to-mass ratio and moment of inertia, increase with the decrease of B eff . Our calculations also show that a 4 significantly affects the stellar rest mass and the total stellar binding energy. As a result, a 4 can have signatures in evolutions of both accreting and non-accreting compact stars, and the observed distribution of stellar mass and spin and other source parameters. Finally, we compute the parameter values of two important pulsars, PSR J1614-2230 and PSR J1748-2446ad, which may have implications to probe their evolutionary histories, and for constraining EoS models.

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Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Fast spinning strange stars: possible ways to constrain interacting quark matter parameters

Bhattacharyya

Bombaci

Logoteta

et al. 2016

Mon. Not. R. Astron. Soc.

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“…So far, various observational attempts to measure M and R have been carried out, and generally yielded M ≃ 1.4M⊙ and R ≃ 12 km (e.g. reviews by Bhattacharyya 2010Bhattacharyya andÖzel 2013. However, the measurements are not yet accurate enough to constrain the EOS.…”

Section: Introductionmentioning

confidence: 99%

Application of the Ghosh & Lamb relation to the spin-up/down behavior in the X-ray binary pulsar 4U 1626−67

Takagi

Mihara

Sugizaki

et al. 2016

Publications of the Astronomical Society of Japan

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We analyzed continuous MAXI/GSC data of the X-ray binary pulsar 4U 1626-67 from 2009 October to 2013 September, and determined the pulse period and the pulse-period derivative for every 60-d interval by the epoch folding method. The obtained periods are consistent with those provided by the Fermi/GBM pulsar project. In all the 60-d intervals, the pulsar was observed to spin up, with the spin-up rate positively correlated with the 2-20 keV flux. We applied the accretion torque model proposed by Ghosh & Lamb (1979, ApJ, 234, 296) to the MAXI/GSC data, as well as the past data including both spin-up and spin-down phases. The Ghosh & Lamb relation was confirmed to successfully explain the observed relation between the spin-up/down rate and the flux. By comparing the model-predicted luminosity with the observed flux, the source distance was constrained as 5-13 kpc, which is consistent with that by Chakrabarty (1998, ApJ, 492, 342). Conversely, if the source distance is assumed, the data can constrain the mass and radius of the neutron star, because the Ghosh & Lamb model depends on these parameters. We attempted this idea, and found that an assumed distance of, e.g., 10 kpc gives a mass in the range of 1.81-1.90 solar mass, and a radius of 11.4-11.5 km, although these results are still subject to considerable systematic uncertainties other than that in the distance.

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“…erties, accretion-powered pulsations, kilo-Hertz quasiperiodic oscillations (kHz QPOs), broad relativistic iron lines, quiescent emissions and timing features due to orbital motion, as complementary tools to reliably measure neutron star parameters (Bhattacharyya 2010). Here, we focus on one of these methods, the one involving the broad relativistic iron line.…”

Section: Introductionmentioning

confidence: 99%

Relativistic Disc Line: A Tool to Constrain Neutron Star Equation of State Models

Bhattacharyya

2017

J Astrophys Astron

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Abstract. Relativistic iron Kα spectral emission line from the inner disc of a neutron star low-mass X-ray binary (LMXB) was first detected in 2007. This discovery opened up new ways to probe strong gravity and dense matter. The past decade has seen detections of such a line from many neutron star LMXBs, and confirmation of this line from the same source with several X-ray satellites. These have firmly established the new field of relativistic disc line from neutron star systems in only ten years. Fitting the shape of such a line with an appropriate general relativistic model provides the accretion disc inner edge radius to the stellar mass ratio. In this review, we briefly discuss how an accurate measurement of this ratio with a future larger area X-ray instrument can be used to constrain neutron star equation of state models.

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Measurement of neutron star parameters: A review of methods for low-mass X-ray binaries

Cited by 68 publications

References 245 publications

Fast spinning strange stars: possible ways to constrain interacting quark matter parameters

Fast spinning strange stars: possible ways to constrain interacting quark matter parameters

Application of the Ghosh & Lamb relation to the spin-up/down behavior in the X-ray binary pulsar 4U 1626−67

Relativistic Disc Line: A Tool to Constrain Neutron Star Equation of State Models

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