The Inclination Angle and Mass of the Black Hole in XTE J1118+480

Balman, Ş.; Kızıloğlu, Ü.; Yılmaz, A.; Kalemci, Emrah; Tomsick, John A.; Bandyopadhyay, Reba M.; Wachter, Stefanie; Gelino, Dawn; Gelino, Christopher R.

doi:10.1063/1.2945095

Cited by 5 publications

(4 citation statements)

References 10 publications

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“…(35) for EOSs previously cited as supporting masses greater than about 1.6 M is reasonably tight. This relation may be inverted to yield a radius estimate given I and M. Furthermore, since I ∝ R 2 , the inferred relative error of R using this procedure would be approximately half the relative measured error of I itself.…”

Section: Moments Of Inertiamentioning

confidence: 81%

Neutron star observations: Prognosis for equation of state constraints

2007

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We investigate how current and proposed observations of neutron stars can lead to an understanding of the state of their interiors and the key unknowns: the typical neutron star radius and the neutron star maximum mass. We consider observations made not only with photons, ranging from radio waves to X-rays, but also those involving neutrinos and gravity waves. We detail how precision determinations of structural properties would lead to significant restrictions on the poorly understood equation of state near and beyond the equilibrium density of nuclear matter.To begin, a theoretical analysis of neutron star structure, including general relativistic limits to mass, compactness, and spin rates is made. A review is the made of recent observations such as pulsar timing (which leads to mass, spin period, glitch and moment of inertia estimates), optical and X-ray observations of cooling neutron stars (which lead to estimates of core temperatures and ages and inferences about the internal composition), and X-ray observations of accreting and bursting sources (which shed light on both the crustal properties and internal composition). Next, we discuss neutrino emission from proto-neutron stars and how neutrino observations of a supernova, from both current and planned detectors, might impact our knowledge of the interiors, mass and radii of neutron stars. We also explore the question of how superstrong magnetic fields could affect the equation of state and neutron star structure. This is followed by a look at binary mergers involving neutron stars and how the detection of gravity waves could unambiguously distinguish normal neutron stars from self-bound strange quark matter stars.

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Section: Moments Of Inertiamentioning

confidence: 81%

Neutron star observations: Prognosis for equation of state constraints

2007

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“…1), we included 55 NSs with error bars varying between 0.009 and 0.548 M ⊙ in our work. The full references to the original works, including the label letter employed in the compilation are given in the reference list (van Kerkwijck, van Paradijs & Zuiderwijck 1995; Barziv et al 2001; Lange et al 2001; Nice, Splaver & Stairs 2001, 2003, 2004; Stairs et al 2002; Freire et al 2003, 2008b; Gelino, Tomsick & Heindl 2003; Jonker, van der Klis & Groot 2003; Quaintrell et al 2003; Corongiu et al 2004; Podsiadlowski et al 2004; Champion et al 2005; Ransom et al 2005; Splaver et al 2005; Weisberg & Taylor 2005; Bassa et al 2006; Hotan, Bailes & Ord 2006; Jacoby et al 2006; Kramer et al 2006; Lorimer et al 2006; Freire, Ransom & Gupta 2007; Steeghs & Jonker 2007; Bhat, Bailes & Verbiest 2008; Ferdman 2008; Freire, Jacoby & Bailes 2008a; Janssen et al 2008; Nice, Stairs & Kasian 2008; Verbiest et al 2008; Freire 2009; Casares et al 2010; Mason et al 2010). The uncertainties for each mass are quite different because the methods of measurement were distinct at different times, and the methods had been improved in many cases.…”

Section: Neutron Star Samplementioning

confidence: 99%

On the mass distribution of neutron stars

Valentim¹,

Rangel²,

Horvath³

2011

Monthly Notices of the Royal Astronomical Society

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The distribution of masses for neutron stars is analyzed using the Bayesian statistical inference, evaluating the likelihood of proposed gaussian peaks by using fifty-four measured points obtained in a variety of systems. The results strongly suggest the existence of a bimodal distribution of the masses, with the first peak around $1.37 {M_{\odot}}$, and a much wider second peak at $1.73 {M_{\odot}}$. The results support earlier views related to the different evolutionary histories of the members for the first two peaks, which produces a natural separation (even if no attempt to "label" the systems has been made here), and argues against the single-mass scale viewpoint. The bimodal distribution can also accommodate the recent findings of $\sim M_{\odot}$ masses quite naturally. Finally, we explore the existence of a subgroup around $1.25 {M_{\odot}}$, finding weak, if any, evidence for it. This recently claimed low-mass subgroup, possibly related to $O-Mg-Ne$ core collapse events, has a monotonically decreasing likelihood and does not stand out clearly from the rest of the sample.Comment: 11 pp., 3 figures, submitted to MNRAS Letter

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“…Uncertainties related to the contamination of the optical lightcurve by the accretion disk [7] and to the spectral characterization of the companion star [11] typically limit the accuracy of the measurements. Here I use the rather optimistic values quoted in reference [12] rather than the more conservative estimates of reference [7]. Having made the opposite choice would have affected only marginally the final result, the accuracy of which is mostly determined by the uncertainty in the radial velocity measurement.…”

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confidence: 99%

Constraints on Braneworld Gravity Models from a Kinematic Limit on the Age of the Black Hole XTEJ1118+480

Psaltis

2007

Phys. Rev. Lett.

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In braneworld gravity models with a finite anti-de Sitter space (AdS) curvature in the extra dimension, the AdS/conformal field theory correspondence leads to a prediction for the lifetime of astrophysical black holes that is significantly smaller than the Hubble time, for asymptotic curvatures that are consistent with current experiments. Using the recent measurements of the position, three-dimensional spatial velocity, and mass of the black hole XTE J1118+480, I calculate a lower limit on its kinematic age of > or =11 Myr (95% confidence). This translates into an upper limit for the asymptotic AdS curvature in the extra dimensions of <0.08 mm, which significantly improves the limit obtained by table top experiments of sub mm gravity.

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The Inclination Angle and Mass of the Black Hole in XTE J1118+480

Cited by 5 publications

References 10 publications

Neutron star observations: Prognosis for equation of state constraints

Neutron star observations: Prognosis for equation of state constraints

On the mass distribution of neutron stars

Constraints on Braneworld Gravity Models from a Kinematic Limit on the Age of the Black Hole XTEJ1118+480

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