bib1.bib

@comment{x-kbibtex-personnameformatting=<%l><, %f>}

@article{poutaviironen,
	abstract = "We study theoretical X-ray light curves and polarization properties of accretion-powered millisecond pulsars. We assume that the radiation is produced in two antipodal spots at the neutron star surface which are associated with the magnetic poles. We compute the angle-dependent intensity and polarization produced in an electron-scattering dominated plane-parallel accretion shock in the frame of the shock. The observed flux, polarization degree and polarization angle are calculated accounting for special and general relativistic effects. The calculations also extended to the case of nuclear-powered millisecond pulsars -- X-ray bursts. In this case, we consider one spot and the radiation is assumed to be produced in the atmosphere of the infinite Thomson optical depth. The light curves and polarization profiles show a large diversity depending on the model parameters. Presented results can be used as a first step to understand the observed pulse profiles of accretion- and nuclear-powered millisecond pulsars. Future observations of the X-ray polarization will provide a valuable tool to test the geometry of the emission region and its physical characteristics.",
	archiveprefix = "arXiv",
	author = "Viironen, Kerttu and Poutanen, Juri",
	comment = "published = 2004-08-13T10:46:36Z, updated = 2004-08-13T10:46:36Z, 14 pages, 11 figures, A\&amp;A, in press",
	doi = "10.1051/0004-6361:20041084",
	eprint = "astro-ph/0408250v1",
	journal = "Astron. Astrophys., 426, 985-997",
	month = aug,
	primaryclass = "astro-ph",
	title = "{Light curves and polarization of accretion- and nuclear-powered millisecond pulsars}",
	url = "http://arxiv.org/abs/astro-ph/0408250v1; http://arxiv.org/pdf/astro-ph/0408250v1",
	x-fetchedfrom = "arXiv.org",
	year = "2004"
}

@article{poutabelo,
	abstract = "Approximate analytical formulae are derived for the pulse profile produced by small hot spots on a rapidly rotating neutron star. Its Fourier amplitudes and phases are calculated. The proposed formalism takes into account gravitational bending of light, Doppler effect, anisotropy of emission, and time delays. Its accuracy is checked with exact numerical calculations.",
	archiveprefix = "arXiv",
	author = "Poutanen, Juri and Beloborodov, Andrei M.",
	comment = "published = 2006-08-30T14:57:20Z, updated = 2006-11-23T09:42:59Z, 9 pages, 6 figures; replaced with the version published in MNRAS",
	doi = "10.1111/j.1365-2966.2006.11088.x",
	eprint = "astro-ph/0608663v2",
	journal = "MNRAS, 373, 836-844",
	month = nov,
	primaryclass = "astro-ph",
	title = "{Pulse profiles of millisecond pulsars and their Fourier amplitudes}",
	url = "http://arxiv.org/abs/astro-ph/0608663v2; http://arxiv.org/pdf/astro-ph/0608663v2",
	x-fetchedfrom = "arXiv.org",
	year = "2006"
}

@article{poutarew2006,
	abstract = "I review X-ray observations of accretion-powered millisecond pulsars and current theories for formation of their spectra and pulse profiles.",
	archiveprefix = "arXiv",
	author = "Poutanen, Juri",
	comment = {published = 2005-10-03T11:58:33Z, updated = 2006-05-17T18:15:48Z, 14 pages, 6 figures; invited review presented at COSPAR Colloquium "Spectra \&amp; Timing of Compact X-ray Binaries", January 17-20, 2005, Mumbai, India. Advances in Space Research, in press},
	doi = "10.1016/j.asr.2006.04.025",
	eprint = "astro-ph/0510038v2",
	journal = "Adv. SpaceRes., 38, 2697-2703",
	month = may,
	primaryclass = "astro-ph",
	title = "{Accretion-powered millisecond pulsars}",
	url = "http://arxiv.org/abs/astro-ph/0510038v2; http://arxiv.org/pdf/astro-ph/0510038v2",
	x-fetchedfrom = "arXiv.org",
	year = "2006"
}

@article{miller,
	abstract = "Simultaneous, precise measurements of the mass $M$ and radius $R$ of neutron stars can yield uniquely valuable information about the still uncertain properties of cold matter at several times the density of nuclear matter. One method that could be used to measure $M$ and $R$ is to analyze the energy-dependent waveforms of the X-ray flux oscillations seen during some thermonuclear bursts from some neutron stars. These oscillations are thought to be produced by X-ray emission from hotter regions on the surface of the star that are rotating at or near the spin frequency of the star. Here we explore how well $M$ and $R$ could be determined by generating, and analyzing using Bayesian techniques, synthetic energy-resolved X-ray data that we produce assuming a future space mission having 2--30 keV energy coverage and an effective area of 10 m$^2$, such as the proposed \textit{LOFT} or \textit{AXTAR} missions. We find that if the hot spot is within 10$^\circ$ of the rotation equator, both $M$ and $R$ can usually be determined with an uncertainty of about 10\% if there are $10^6$ total counts from the spot, whereas waveforms from spots within 20$^\circ$ of the rotation pole provide no useful constraints. These constraints can usually be achieved even if the burst oscillations vary with time and data from multiple bursts must be used to obtain 10$^6$ counts from the hot spot. This is therefore a promising method to constrain $M$ and $R$ tightly enough to discriminate strongly between competing models of cold, high-density matter.",
	archiveprefix = "arXiv",
	author = "Lo, Ka-Ho and Miller, M. Coleman and Bhattacharyya, Sudip and Lamb, Frederick K.",
	comment = "published = 2013-04-08T19:38:56Z, updated = 2013-04-08T19:38:56Z, 73 pages, including 26 figures and 8 tables. Submitted to The Astrophysical Journal",
	doi = "10.1088/0004-637X/776/1/19",
	eprint = "1304.2330v1",
	journal = "Astrophys. J., 776, 1, 19, 38",
	month = apr,
	primaryclass = "astro-ph.HE",
	title = "{Determining neutron star masses and radii using energy-resolved waveforms of X-ray burst oscillations}",
	url = "http://arxiv.org/abs/1304.2330v1; http://arxiv.org/pdf/1304.2330v1",
	x-fetchedfrom = "arXiv.org",
	year = "2013"
}

@article{morsink,
	abstract = "We present a simple method for including the oblateness of a rapidly rotating neutron star when fitting X-ray light curves. In previous work we showed that the oblateness induced by rotation at frequencies above 300 Hz produces a geometric effect which needs to be accounted for when modelling light curves to extract constraints on the neutron star's mass and radius. In our model X-rays are emitted from the surface of an oblate neutron star and propagate to the observer along geodesics of the Schwarzschild metric for a spherical neutron star. Doppler effects due to rotation are added in the same manner as in the case of a spherical neutron star. We show that this model captures the most important effects due to the neutron star's rotation. We also explain how the geometric oblateness effect can rival the Doppler effect for some emission geometries.",
	archiveprefix = "arXiv",
	author = "Morsink, Sharon M. and Leahy, Denis A. and Cadeau, Coire and Braga, John",
	comment = "published = 2007-03-06T18:32:44Z, updated = 2007-04-05T19:23:34Z, 8 pages, 4 figures. v2: minor changes. Accepted by the Astrophysical Journal",
	doi = "10.1086/518648",
	eprint = "astro-ph/0703123v2",
	journal = "Astrophys. J., 663, 1244-1251",
	month = apr,
	primaryclass = "astro-ph",
	title = "{The Oblate Schwarzschild Approximation for Light Curves of Rapidly Rotating Neutron Stars}",
	url = "http://arxiv.org/abs/astro-ph/0703123v2; http://arxiv.org/pdf/astro-ph/0703123v2",
	x-fetchedfrom = "arXiv.org",
	year = "2007"
}

@article{cadeau,
	abstract = "We present raytracing computations for light emitted from the surface of a rapidly-rotating neutron star in order to construct light curves for X-ray pulsars and bursters. These calculations are for realistic models of rapidly-rotating neutron stars which take into account both the correct exterior metric and the oblate shape of the star. We find that the most important effect arising from rotation comes from the oblate shape of the rotating star. We find that approximating a rotating neutron star as a sphere introduces serious errors in fitted values of the star's radius and mass if the rotation rate is very large. However, in most cases acceptable fits to the ratio M/R can be obtained with the spherical approximation.",
	archiveprefix = "arXiv",
	author = "Cadeau, Coire and Morsink, Sharon M. and Leahy, Denis and Campbell, Sheldon S.",
	comment = "published = 2006-09-12T15:21:50Z, updated = 2006-09-12T15:21:50Z, Accepted by the Astrophysical Journal. 13 pages \&amp; 7 figures",
	doi = "10.1086/509103",
	eprint = "astro-ph/0609325v1",
	journal = "Astrophys. J., 654, 458-469",
	month = sep,
	primaryclass = "astro-ph",
	title = "{Light Curves for Rapidly-Rotating Neutron Stars}",
	url = "http://arxiv.org/abs/astro-ph/0609325v1; http://arxiv.org/pdf/astro-ph/0609325v1",
	x-fetchedfrom = "arXiv.org",
	year = "2006"
}

@article{nattila_bayes,
	abstract = "The cooling phase of thermonuclear (type-I) X-ray bursts can be used to constrain the neutron star (NS) compactness by comparing the observed cooling tracks of bursts to accurate theoretical atmosphere model calculations. By applying the so-called cooling tail method, where the information from the whole cooling track is used, we constrain the mass, radius, and distance for three different NSs in low-mass X-ray binaries 4U 1702-429, 4U 1724-307, and SAX J1810.8-260. Care is taken to only use the hard state bursts where it is thought that only the NS surface alone is emitting. We then utilize a Markov chain Monte Carlo algorithm within a Bayesian framework to obtain a parameterized equation of state (EoS) of cold dense matter from our initial mass and radius constraints. This allows us to set limits on various nuclear parameters and to constrain an empirical pressure-density relation for the dense matter. Our predicted EoS results in NS radius between 10.5-12.8 km (95\% confidence limits) for a mass of 1.4 $M_{\odot}$. Due to systematic errors and uncertainty in the composition these results should be interpreted as lower limits for the radius.",
	archiveprefix = "arXiv",
	author = "N{\"a}ttil{\"a}, J. and Steiner, A. W. and Kajava, J. J. E. and Suleimanov, V. F. and Poutanen, J.",
	comment = "published = 2015-09-22T12:09:47Z, updated = 2016-03-15T13:01:13Z, 23 pages, 12 figures, revised version, accepted for publication in A\&amp;A",
	doi = "10.1051/0004-6361/201527416",
	eprint = "1509.06561v2",
	journal = "Astron. Astrophys., 591, A25, 23",
	month = mar,
	primaryclass = "astro-ph.HE",
	title = "{Equation of state constraints for the cold dense matter inside neutron stars using the cooling tail method}",
	url = "http://arxiv.org/abs/1509.06561v2; http://arxiv.org/pdf/1509.06561v2",
	x-fetchedfrom = "arXiv.org",
	year = "2016"
}


@article{algendy,
	abstract = "On the surface of a rapidly rotating neutron star, the effective centrifugal force decreases the effective acceleration due to gravity (as measured in the rotating frame) at the equator while increasing the acceleration at the poles due to the centrifugal flattening of the star into an oblate spheroid. We compute the effective gravitational acceleration for relativistic rapidly rotating neutron stars and show that for a star with mass $M$, equatorial radius $R_e$, and angular velocity $\Omega$, the deviations of the effective acceleration due to gravity from the nonrotating case take on a universal form that depends only on the compactness ratio $M/R_e$, the dimensionless square of the angular velocity $\Omega^2R_e^3/GM$, and the latitude on the star's surface. This dependence is universal, in that it has very little dependence on the neutron star's equation of state. The effective gravity is expanded in the slow rotation limit to show the dependence on the effective centrifugal force, oblate shape of the star and the quadrupole moment of the gravitational field. In addition, an empirical fit and simple formula for the effective gravity is found. We find that the increase in the acceleration due to gravity at the poles is of the same order of magnitude as the decrease in the effective acceleration due to gravity at the equator for all realistic value of mass, radius and spin. For neutron stars that spin with frequencies near 600 Hz the difference between the effective gravity at the poles and the equator is about 20\%.",
	archiveprefix = "arXiv",
	author = "AlGendy, Mohammad and Morsink, Sharon M.",
	comment = "published = 2014-04-02T16:46:18Z, updated = 2014-04-02T16:46:18Z, 13 pages, 3 figures",
	doi = "10.1088/0004-637X/791/2/78",
	eprint = "1404.0609v1",
	journal = "Astrophys. J., 791, 2, 78, 11 ",
	month = apr,
	primaryclass = "astro-ph.HE",
	url = "http://arxiv.org/abs/1404.0609v1; http://arxiv.org/pdf/1404.0609v1",
	x-fetchedfrom = "arXiv.org",
	year = "2014"
}

@book{mtw,
	author = "Misner, Ch.W. and Thorne, K.S. and Wheeler, J.A.",
	publisher = "W. Freeman",
	title = "{Gravitation}",
	year = 1973
}

@article{lattimer,
	abstract = "Neutron stars are some of the densest manifestations of massive objects in the universe. They are ideal astrophysical laboratories for testing theories of dense matter physics and provide connections among nuclear physics, particle physics and astrophysics. Neutron stars may exhibit conditions and phenomena not observed elsewhere, such as hyperon-dominated matter, deconfined quark matter, superfluidity and superconductivity with critical temperatures near ${10^{10}}$ kelvin, opaqueness to neutrinos, and magnetic fields in excess of $10^{13}$ Gauss. Here, we describe the formation, structure, internal composition and evolution of neutron stars. Observations that include studies of binary pulsars, thermal emission from isolated neutron stars, glitches from pulsars and quasi-periodic oscillations from accreting neutron stars provide information about neutron star masses, radii, temperatures, ages and internal compositions.",
	archiveprefix = "arXiv",
	author = "Lattimer, J. M. and Prakash, M.",
	comment = "published = 2004-05-13T17:54:43Z, updated = 2004-05-13T17:54:43Z, 22 pages, 4 figures and 1 table",
	doi = "10.1126/science.1090720",
	eprint = "astro-ph/0405262v1",
	journal = "Science, 304, 536-542",
	month = may,
	primaryclass = "astro-ph",
	title = "{The Physics of Neutron Stars}",
	url = "http://arxiv.org/abs/astro-ph/0405262v1; http://arxiv.org/pdf/astro-ph/0405262v1",
	x-fetchedfrom = "arXiv.org",
	year = "2004"
}

@article{rhoades,
	author = "Rhoades, C.E. and Ruffini, R.",
	journal = "Phys. Rev. Lett., 32, 324",
	title = "{Maximum Mass of a Neutron Star}",
	year = "1974"
}

@article{patruno,
	added-at = "2013-05-12T07:23:46.000+0200",
	adsnote = "Provided by the SAO/NASA Astrophysics Data System",
	adsurl = "http://adsabs.harvard.edu/abs/2012arXiv1206.2727P",
	archiveprefix = "arXiv",
	author = "{Patruno}, A. and {Watts}, A. L.",
	eprint = "1206.2727",
	interhash = "31583b24c74636e7b72b10e2f6895acb",
	intrahash = "739cf49d37b155e6b250fbc14c9d5bf4",
	journal = "arXiv:1206.2727",
	keywords = "thesis 1023-timing-paper lmxb amxp",
	month = jun,
	primaryclass = "astro-ph.HE",
	timestamp = "2013-05-12T07:23:46.000+0200",
	title = "{Accreting Millisecond X-Ray Pulsars}",
	url = "http://www.bibsonomy.org/bibtex/2739cf49d37b155e6b250fbc14c9d5bf4/aarchiba",
	x-fetchedfrom = "Bibsonomy",
	year = 2012
}

@article{twocompmod,
	author = "{Gierli\'{n}ski}, M. and Done, C. and Barret, D.",
	journal = "MNRAS, 331, 141",
	title = "{Phase-resolved X-ray spectroscopy of the millisecond pulsar SAX J1808.4---3658}",
	year = "2002"
}

@article{pechenick,
	author = "Pechenick, K. R. and Ftaclas, C. and Cohen, J. M.",
	journal = "Astrophys. J., 274, 846-857",
	title = "{Hot spots on neutron stars - The near-field gravitational lens}",
	year = "1983"
}

@article{poutagierlinskisax,
	abstract = {The pulse profiles of the accreting X-ray millisecond pulsar SAX J1808.4-3658 at different energies are studied. The two main emission component, the black body and the Comptonized tail that are clearly identified in the time-averaged spectrum, show strong variability with the first component lagging the second one. The observed variability can be explained if the emission is produced by Comptonization in a hot slab (radiative shock) of Thomson optical depth ~0.3-1 at the neutron star surface. The emission patterns of the black body and the Comptonized radiation are different: a "knife"- and a "fan"-like, respectively. We construct a detailed model of the X-ray production accounting for the Doppler boosting, relativistic aberration and gravitational light bending in the Schwarzschild spacetime. We present also accurate analytical formulae for computations of the light curves from rapidly rotating neutron stars using formalism recently developed by Beloborodov (2002). Our model reproduces well the pulse profiles at different energies simultaneously, corresponding phase lags, as well as the time-averaged spectrum. We constrain the compact star mass to be bounded between 1.2 and 1.6 solar masses. By fitting the observed profiles, we determine the radius of the compact object to be R~11 km if M=1.6 M\_sun, while for M=1.2 M\_sun the best-fitting radius is ~6.5 km, indicating that the compact object in SAX J1808.4-3658 can be a strange star. We obtain a lower limit on the inclination of the system of 65 degrees.},
	archiveprefix = "arXiv",
	author = "Poutanen, Juri and Gierli\'{n}ski, Marek",
	comment = "published = 2003-03-04T16:54:23Z, updated = 2003-03-04T16:54:23Z, 11 pages, 7 figures, submitted to MNRAS",
	doi = "10.1046/j.1365-8711.2003.06773.x",
	eprint = "astro-ph/0303084v1",
	journal = "MNRAS, 343, 1301",
	month = mar,
	primaryclass = "astro-ph",
	title = "{On the Nature of the X-ray Emission from the Accreting Millisecond Pulsar SAX J1808.4-3658}",
	url = "http://arxiv.org/abs/astro-ph/0303084v1; http://arxiv.org/pdf/astro-ph/0303084v1",
	x-fetchedfrom = "arXiv.org",
	year = "2003"
}

@article{beloborodov,
	abstract = "A photon emitted near a compact object at an angle $\alpha$ with respect to the radial direction escapes to infinity at a different angle $\psi&gt;\alpha$. This bending of light is caused by a strong gravitational field. We show that, in a Schwarzschild metric, the effect is described by $1-\cos\alpha=(1-\cos\psi)(1-r_g/R)$ where $R/r_g$ is the emission radius in Schwarzschild units. The formula is approximate and it applies at $R\geq 2r_g$ only, however at these radii it has amazing accuracy, fully sufficient in many applications. As one application we develop a new formulation for the light bending effects in pulsars. It reveals the simple character of these effects and gives their quantitative description with practically no losses of accuracy (for the typical radius of a neutron star $R=3r_g$ the error is 1\%). The visible fraction of a star surface is shown to be $S_v/4\pi R^2=[2(1-r_g/R)]^{-1}$ which is 3/4 for $R=3r_g$. The instantaneous flux of a pulsar comes from one or two antipodal polar caps that rotate in the visible zone. The pulse produced by one blackbody cap is found to be sinusoidal (light bending impacts the pulse amplitude but not its shape). When both caps are visible, the pulse shows a plateau: the variable parts of the antipodal emissions precisely cancel each other. The pulsed fraction of blackbody emission with antipodal symmetry has an upper limit $A_{max}=(R-2r_g)/(R+2r_g)$. Pulsars with $A&gt;A_{max}$ must be asymmetric.",
	archiveprefix = "arXiv",
	author = "Beloborodov, Andrei M.",
	comment = "published = 2002-01-08T21:07:49Z, updated = 2002-01-08T21:07:49Z, accepted to ApJ Letters",
	doi = "10.1086/339511",
	eprint = "astro-ph/0201117v1",
	journal = "Astrophys. J., 566, L85-L88",
	month = jan,
	primaryclass = "astro-ph",
	title = "{Gravitational Bending of Light Near Compact Objects}",
	url = "http://arxiv.org/abs/astro-ph/0201117v1; http://arxiv.org/pdf/astro-ph/0201117v1",
	x-fetchedfrom = "arXiv.org",
	year = "2002"
}

@mastersThesis{falkner,
	author = "Falkner, S.",
	title = "{Light Bending around Neutron Stars}",
	year = "Friedrich-Alexander University of Erlangen-Nuremberg (2002)"

}

@mastersThesis{kaiser,
	author = "Kaiser, A. D.",
	title = "{Computational Experiments in Markov Chain Monte Carlo}",
	year = "New York University (2013)"

}

@article{ensemble1,
	author = "Goodman, J. and Weare, J.",
	journal = "Commun. Appl. Math. Comput. Sci., 5, 65-80",
	title = "{Ensemble Samplers with Affine Invariance}",
	year = "2010"
}

@phdThesis{tuomi,
	author = "Tuomi, M.",
	title = "{Multidata inverse problems and Bayesian solution methods in astronomy}",
	year = "University of Turku (2013)"

}

@book{mc_methods_book,
	abstract = "HEIDI",
	added-at = "2009-10-26T17:15:13.000+0100",
	author = "Kalos, Malvin H. and Whitlock, Paula A.",
	biburl = "http://www.bibsonomy.org/bibtex/24e02db0dcc859fdf6f2dee267b1250f6/rhirsch",
	interhash = "3847020e38ad6fa9d6b4620525bb25da",
	intrahash = "4e02db0dcc859fdf6f2dee267b1250f6",
	isbn = "3-527-40760-X, 978-3-527-40760-6",
	keywords = "Monte-Carlo-Simulation",
	language = "eng",
	publisher = "Wiley-VCH",
	timestamp = "2009-10-26T17:15:13.000+0100",
	title = "{Monte Carlo methods}",
	x-fetchedfrom = "Bibsonomy",
	year = 2008
}

@article{emceehammer,
	abstract = "We introduce a stable, well tested Python implementation of the affine-invariant ensemble sampler for Markov chain Monte Carlo (MCMC) proposed by Goodman \&amp; Weare (2010). The code is open source and has already been used in several published projects in the astrophysics literature. The algorithm behind emcee has several advantages over traditional MCMC sampling methods and it has excellent performance as measured by the autocorrelation time (or function calls per independent sample). One major advantage of the algorithm is that it requires hand-tuning of only 1 or 2 parameters compared to $\sim N^2$ for a traditional algorithm in an N-dimensional parameter space. In this document, we describe the algorithm and the details of our implementation and API. Exploiting the parallelism of the ensemble method, emcee permits any user to take advantage of multiple CPU cores without extra effort. The code is available online at http://dan.iel.fm/emcee under the MIT License.",
	archiveprefix = "arXiv",
	author = "Foreman-Mackey, Daniel and Hogg, David W. and Lang, Dustin and Goodman, Jonathan",
	comment = "published = 2012-02-16T20:41:19Z, updated = 2013-11-25T15:56:48Z, Code re-licensed under MIT",
	doi = "10.1086/670067",
	eprint = "1202.3665v4",
	journal = "Publications of the Astronomical Society of Pacific, 125, 925, 306-312",
	month = nov,
	primaryclass = "astro-ph.IM",
	title = "{emcee: The MCMC Hammer}",
	url = "http://arxiv.org/abs/1202.3665v4; http://arxiv.org/pdf/1202.3665v4",
	x-fetchedfrom = "arXiv.org",
	year = "2013"
}

@article{tolman,
	author = "Tolman, R. C.",
	journal = "Proceedings of the National Academy of Science, 20, 169",
	year = "1934"
}

@article{oppenheimer,
	author = "Oppenheimer, J. R. and Volkoff, G. M.",
	journal = "Phys. Rev., 55, 374",
	year = "1939"
}

@article{lindbland85,
	author = "Lind, K. R. and Blandford, R. D.",
	journal = "Astrophys. J., 295, 358-367",
	title = "{Semidynamical models of radio jets - Relativistic beaming and source counts}",
	year = "1985"
}

@article{metropolis53,
	added-at = "2008-04-15T18:39:30.000+0200",
	author = "Metropolis, N. and Rosenbluth, A. and Rosenbluth, M. and Teller, A. and Teller, E.",
	biburl = "http://www.bibsonomy.org/bibtex/2696c7dfcbed67f0382ed02aa803817da/vittorio.loreto",
	interhash = "b67019ed11f34441c67cc69ee5683945",
	intrahash = "696c7dfcbed67f0382ed02aa803817da",
	journal = "J. Chem. Phys.",
	keywords = "1953 metropolis montecarlo rosenbluth RMP\_CFL teller",
	pages = 1087,
	timestamp = "2008-04-15T18:39:31.000+0200",
	title = "{Equation of State Calculations by Fast Computing Machines}",
	volume = 21,
	x-fetchedfrom = "Bibsonomy",
	year = 1953
}

@article{hastings70,
	added-at = "2011-05-09T23:10:52.000+0200",
	author = "Hastings, W. K.",
	biburl = "http://www.bibsonomy.org/bibtex/206f22d1e8d42fd18723a51ac3679b607/josephausterwei",
	interhash = "d8633f8e78c50c1d64136febae25d79d",
	intrahash = "06f22d1e8d42fd18723a51ac3679b607",
	journal = "Biometrika",
	keywords = "imported",
	pages = "97-109",
	timestamp = "2011-05-10T10:42:42.000+0200",
	title = "{Monte {C}arlo methods using {M}arkov chains and their applications}",
	volume = 57,
	x-fetchedfrom = "Bibsonomy",
	year = 1970
}

@article{lattimer2007,
	abstract = "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. A theoretical analysis of neutron star structure, including general relativistic limits to mass, compactness, and spin rates is made. 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.",
	archiveprefix = "arXiv",
	author = "Lattimer, James M. and Prakash, Maddapa",
	comment = "published = 2006-12-15T17:22:23Z, updated = 2006-12-15T17:22:23Z, 70 pages, 19 figures, submitted to Hans Bethe Centennial Physics Reports",
	doi = "10.1016/j.physrep.2007.02.003",
	eprint = "astro-ph/0612440v1",
	journal = "Phys. Rept., 442, 109-165",
	month = dec,
	primaryclass = "astro-ph",
	title = "{Neutron Star Observations: Prognosis for Equation of State Constraints}",
	url = "http://arxiv.org/abs/astro-ph/0612440v1; http://arxiv.org/pdf/astro-ph/0612440v1",
	x-fetchedfrom = "arXiv.org",
	year = "2007"
}

@article{hebeler,
	abstract = "We show that microscopic calculations based on chiral effective field theory interactions constrain the properties of neutron-rich matter below nuclear densities to a much higher degree than is reflected in commonly used equations of state. Combined with observed neutron star masses, our results lead to a radius R = 9.7 - 13.9 km for a 1.4 M\_{solar} star, where the theoretical range is due, in about equal amounts, to uncertainties in many-body forces and to the extrapolation to high densities.",
	archiveprefix = "arXiv",
	author = "Hebeler, K. and Lattimer, J. M. and Pethick, C. J. and Schwenk, A.",
	comment = "published = 2010-07-10T22:02:28Z, updated = 2010-10-26T15:13:48Z, 4 pages, 4 figures; NORDITA-2010-45",
	doi = "10.1103/PhysRevLett.105.161102",
	eprint = "1007.1746v2",
	journal = "Phys. Rev. Lett., 105, 16, 161102",
	month = oct,
	primaryclass = "nucl-th",
	title = "{Constraints on neutron star radii based on chiral effective field theory interactions}",
	url = "http://arxiv.org/abs/1007.1746v2; http://arxiv.org/pdf/1007.1746v2",
	x-fetchedfrom = "arXiv.org",
	year = "2010"
}

@article{lattimer2013,
	abstract = "Neutron stars are valuable laboratories for the study of dense matter. Recent observations have uncovered both massive and low-mass neutron stars and have also set constraints on neutron star radii. The largest mass measurements are powerfully influencing the high-density equation of state because of the existence of the neutron star maximum mass. The smallest mass measurements, and the distributions of masses, have implications for the progenitors and formation mechanisms of neutron stars. The ensemble of mass and radius observations can realistically restrict the properties of dense matter, and, in particular, the behavior of the nuclear symmetry energy near the nuclear saturation density. Simultaneously, various nuclear experiments are progressively restricting the ranges of parameters describing the symmetry properties of the nuclear equation of state. In addition, new theoretical studies of pure neutron matter are providing insights. These observational, experimental and theoretical constraints of dense matter, when combined, are now revealing a remarkable convergence.",
	archiveprefix = "arXiv",
	author = "Lattimer, James M.",
	comment = "published = 2013-05-15T14:59:02Z, updated = 2013-05-15T14:59:02Z, 61 pages including 13 figures",
	doi = "10.1146/annurev-nucl-102711-095018",
	eprint = "1305.3510v1",
	journal = "Annu. Rev. Nucl. Part. Sci., 62, 485",
	month = may,
	primaryclass = "nucl-th",
	title = "{The Nuclear Equation of State and Neutron Star Masses}",
	url = "http://arxiv.org/abs/1305.3510v1; http://arxiv.org/pdf/1305.3510v1",
	x-fetchedfrom = "arXiv.org",
	year = "2013"
}

@article{akmal,
	abstract = "Properties of dense nucleon matter and the structure of neutron stars are studied using variational chain summation methods and the new Argonne v18 two-nucleon interaction. The neutron star gravitational mass limit obtained with this interaction is 1.67 M\_{solar}. Boost corrections to the two-nucleon interaction, which give the leading relativistic effect of order (v/c)^2, as well as three-nucleon interactions, are also included in the nuclear Hamiltonian. Their successive addition increases the mass limit to 1.80 and 2.20 M\_{solar}. Hamiltonians including a three-nucleon interaction predict a transition in neutron star matter to a phase with neutral pion condensation at a baryon number density of 0.2 fm^{-3}. We also investigate the possibility of dense nucleon matter having an admixture of quark matter, described using the bag model equation of state. Neutron stars of 1.4 M\_{solar} do not appear to have quark matter admixtures in their cores. However, the heaviest stars are predicted to have cores consisting of a quark and nucleon matter mixture. These admixtures reduce the maximum mass of neutron stars from 2.20 to 2.02 (1.91) M\_{solar} for bag constant B = 200 (122) MeV/fm^3. Stars with pure quark matter in their cores are found to be unstable. We also consider the possibility that matter is maximally incompressible above an assumed density, and show that realistic models of nuclear forces limit the maximum mass of neutron stars to be below 2.5 M\_{solar}. The effects of the phase transitions on the composition of neutron star matter and its adiabatic index are discussed.",
	archiveprefix = "arXiv",
	author = "Akmal, A. and Pandharipande, V. R. and Ravenhall, D. G.",
	comment = "published = 1998-04-13T21:50:12Z, updated = 1998-04-13T21:50:12Z, 39 pages RevTeX including 12 tables. 21 postscript figures. Submitted to Phys. Rev. C",
	doi = "10.1103/PhysRevC.58.1804",
	eprint = "nucl-th/9804027v1",
	journal = "Phys. Rev., C58, 1804-1828",
	month = apr,
	primaryclass = "nucl-th",
	title = "{The equation of state for nucleon matter and neutron star structure}",
	url = "http://arxiv.org/abs/nucl-th/9804027v1; http://arxiv.org/pdf/nucl-th/9804027v1",
	x-fetchedfrom = "arXiv.org",
	year = "1998"
}

@article{gold68,
	author = "Gold, T.",
	journal = "Nature, 218, 5143, 731-732",
	title = "{Rotating Neutron Stars as the Origin of the Pulsating Radio Sources}",
	year = "1968"
}

@book{frank85,
	author = "Frank, J. and King, A. R. and Raine, D. J.",
	publisher = "Cambridge University Press",
	title = "{Accretion Power in Astrophysics}",
	year = "1985"
}

@article{zandsax1808,
	abstract = "We report the discovery of a fairly bright transient during observations with the Wide Field Cameras on board the BeppoSAX satellite in September 1996. It was detected at a peak intensity of 0.1 Crab (2 to 10 keV) and lasted between 6 and 40 days above a detection threshold of 2 mCrab. Two very bright type I X-ray bursts were detected from this transient in the same observations. These almost certainly identify this X-ray transient as a low-mass X-ray binary with a neutron star as compact component. The double-peaked time history of both bursts at high energies suggests a peak luminosity close to the Eddington limit. Assuming this to be true implies a distance to this object of 4 kpc.",
	archiveprefix = "arXiv",
	author = "in 't Zand, J. J. M. and Heise, J. and Muller, J. M. and Bazzano, A. and Cocchi, M. and Natalucci, L. and Ubertini, P.",
	comment = "published = 1998-02-09T08:34:03Z, updated = 1998-02-09T08:34:03Z, 4 pages, 4 figures, published in A\&amp;A March II 1998 issue",
	eprint = "astro-ph/9802098v1",
	journal = "Astron. Astrophys., 331, L25-L28",
	month = feb,
	primaryclass = "astro-ph",
	title = "{Discovery of the X-ray transient SAX J1808.4-3658, a likely low mass X-ray binary}",
	url = "http://arxiv.org/abs/astro-ph/9802098v1; http://arxiv.org/pdf/astro-ph/9802098v1",
	x-fetchedfrom = "arXiv.org",
	year = "1998"
}

@article{wijnandssax1808,
	author = "Wijnands, R. and {van der Klis}, M.",
	journal = "Nature, 394, 6691, 344-346",
	title = "{A millisecond pulsar in an X-ray binary system}",
	year = "1998"
}

@article{madej,
	abstract = "We analyzed archival X-ray spectra of MXB 1728-34 obtained in 1996-99 by the Proportional Counter Array on board of the RXTE satellite. X-ray spectra were fitted to our extensive grids of model atmosphere spectra to determine the effective temperature T\_eff on the neutron star surface, logarithm of surface gravity log(g), and the gravitational redshift z simultaneously. We have chosen fitting by numerical model spectra plus broad Gaussian line, modified by interstellar absorption and the absorption on dust. We arbitrarily assumed either hydrogen-helium chemical composition of a model atmosphere, or H-He-Fe mixture in solar proportion. The statistically best values of log(g), and z subsequently were used to determine mass and radius of the neutron star. We obtained the best values of the parameters for the neutron star in X-ray burst source MXB 1728-34: mass either M=0.40 or 0.63 M\_sol (for H-He or H-He-Fe models, respectively), radius R=4.6 or 5.3 km, log(g)=14.6 or 14.6 and the gravitational redshift z=0.14 or 0.22. All the above parameters have very wide 1-sigma confidence limits. Their values strongly support the equation of state for strange matter in MXB 1728-34.",
	archiveprefix = "arXiv",
	author = "Majczyna, A. and Madej, J.",
	comment = "published = 2006-01-04T12:39:12Z, updated = 2006-01-04T12:39:12Z, Acta Astonomica in print",
	eprint = "astro-ph/0601076v1",
	journal = "Acta Astron., 55, 1-16",
	month = jan,
	primaryclass = "astro-ph",
	title = "{Mass and radius determination for the neutron star in X-ray burst source 4U/MXB 1728-34}",
	url = "http://arxiv.org/abs/astro-ph/0601076v1; http://arxiv.org/pdf/astro-ph/0601076v1",
	x-fetchedfrom = "arXiv.org",
	year = "2006"
}

@article{millerlamb98,
	abstract = "The discovery of high-amplitude brightness oscillations at the spin frequency or its first overtone in six neutron stars in low-mass X-ray binaries during type~1 X-ray bursts provides a powerful new way to constrain the compactness of these stars, and hence to constrain the equation of state of the dense matter in all neutron stars. Here we present the results of general relativistic calculations of the maximum fractional rms amplitudes that can be observed during bursts. In particular, we determine the dependence of the amplitude on the compactness of the star, the angular dependence of the emission from the surface, the rotational velocity at the stellar surface, and whether there are one or two emitting poles. We show that if two poles are emitting, as is strongly indicated by independent evidence in 4U 1636-536 and KS 1731-26, the resulting limits on the compactness of the star can be extremely restrictive. We also discuss the expected amplitudes of X-ray color oscillations and the observational signatures necessary to derive convincing constraints on neutron star compactness from the amplitudes of burst oscillations.",
	archiveprefix = "arXiv",
	author = "Miller, M. Coleman and Lamb, Frederick K.",
	comment = "published = 1997-11-26T21:38:43Z, updated = 1997-11-26T21:38:43Z, 8 pages plus one figure, AASTeX v. 4.0, submitted to The Astrophysical Journal Letters",
	doi = "10.1086/311335",
	eprint = "astro-ph/9711325v1",
	journal = "Astrophys. J., 499, L37",
	month = nov,
	primaryclass = "astro-ph",
	title = "{Bounds on the Compactness of Neutron Stars from Brightness Oscillations}",
	url = "http://arxiv.org/abs/astro-ph/9711325v1; http://arxiv.org/pdf/astro-ph/9711325v1",
	x-fetchedfrom = "arXiv.org",
	year = "1998"
}


@book{lightman75,
	author = "Lightman, A. P. and Press, W. H. and Price, R. H. and Teukolsky, S. A.", 
	publisher = "Princeton University Press",
	title = "{Problem book in relativity and gravitation}",
	year = "1975"
}

@article{Terrell,
	author = "Terrell, J.",
	journal = "Phys. Rev., 116, 1041",
	title = "{Invisibility of the Lorentz Contraction}",
	year = "1959"
}

@book{rybicki,
	author = "Rybicki, G. B. and Lightman, A. P.",
	publisher = "Wiley-Interscience",
	title = "{Radiative Processes in Astrophysics}",
	year = "1979"
}

@article{lattimer2001,

	author = "Lattimer, James M. and Prakash, Maddapa",
	journal = "Astrophys. J., 550, 426-442",
	title = "{NEUTRON STAR STRUCTURE AND THE EQUATION OF STATE}",
	year = "2001"
}

@article{link1999,

	author = "Link, B. and Epstein, R. I. and Lattimer, J. M.",
	journal = "Phys. Rev. Lett., 83, 17, 3362-3365",
	title = "{Pulsar Constraints on Neutron Star Structure and Equation of State}",
	year = "1999"
}


@article{demorest,

	author = "Demorest, P. and Pennucci, T. and Ransom, S. and Roberts, M. and Hessels, J. W. T.",
	journal = "Nature, 467, 7319, 1081-1083",
	title = "{Shapiro delay measurement of a 2 solar mass neutron star}",
	year = "2010"
}


@article{outburst,

	author = "Sanna, A. and Burderi, L. and Riggio, A. and Pintore, F. and Di Salvo, T. and Gambino, A. F. and Iaria, R. and Matranga, M. and Scarano, F.",
	journal = "MNRAS, 459, 2, 1340-1349",
	title = "{Timing of the accreting millisecond pulsar SAX J1748.9−2021 during its 2015 outburst}",
	year = "2016"
}


@article{romanova,
	author = "Romanova, M. M. and Ustyugova, G. V. and Koldoba, A. V. and Lovelace, R. V. E.",
	journal = "Astrophys. J., 610, 920-932",
	title = "{THREE-DIMENSIONAL SIMULATIONS OF DISK ACCRETION TO AN INCLINED DIPOLE. II. HOT SPOTS AND VARIABILITY}",
	year = "2004"
}


@article{disc-instability,
	author = "Lasota, Jean-Pierre",
	journal = "New Astronomy Reviews, 45, 7, 449-508",
	title = "{The disc instability model of dwarf novae and low-mass X-ray binary transients}",
	year = "2001"
}

@article{millerlamb2015,
	author = "Miller, M. Coleman and Lamb, Frederick K.",
	journal = "Astrophys. J., 808, 1, 31, 20",
	title = "{Determining Neutron Star Properties by Fitting Oblate-star Waveform Models to X-Ray Burst Oscillations}",
	year = "2015"
}


@article{savgol,
	author = "Savitzky, A. and Golay, M. J. E",
	journal = "Anal. Chem., 36, 1627-1639",
	title = "{Smoothing and differentiation of data by simplified least squares procedures}",
	year = "1964"
}