Relevant bibliographies by topics / Neutron stars masses

Academic literature on the topic 'Neutron stars masses'

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Published: 9 March 2023
Last updated: 10 March 2023

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Journal articles on the topic "Neutron stars masses"

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Horvath, Jorge Ernesto, Lívia S. Rocha, Antonio Bernardo, Rodolfo Valientim, and Marcio Guilherme Bronzato Avellar. "Neutron stars origins and masses." Astronomische Nachrichten 342, no. 1-2 (January 2021): 294–99. http://dx.doi.org/10.1002/asna.202113922.

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Kreim, S., M. Hempel, D. Lunney, and J. Schaffner-Bielich. "Nuclear masses and neutron stars." International Journal of Mass Spectrometry 349-350 (September 2013): 63–68. http://dx.doi.org/10.1016/j.ijms.2013.02.015.

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Beck, D. H. "Neutron decay, dark matter and neutron stars." EPJ Web of Conferences 219 (2019): 05006. http://dx.doi.org/10.1051/epjconf/201921905006.

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Following up on a suggestion that decay to a dark matter fermion might explain the 4σ discrepancy in the neutron lifetime, we consider the implications of such a fermion on neutron star structure. We find that including it reduces the maximum neutron star mass to well below the observed masses. In order to recover stars with the observed masses, the (repulsive) self-interactions of the dark fermion would have to be stronger than those of the nucleon-nucleon interaction.
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de Souza, Gibran H., Ernesto Kemp, and Cecilia Chirenti. "Magnetized Neutron Stars." International Journal of Modern Physics: Conference Series 45 (January 2017): 1760032. http://dx.doi.org/10.1142/s2010194517600321.

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In this work we show the results for numerical solutions of the relativistic Grad-Shafranov equation for a typical neutron star with 1.4 solar masses. We have studied the internal magnetic field considering both the poloidal and toroidal components, as well as the behavior of the field lines parametrized by the ratio between these components of the field.
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MENEZES, DÉBORA P., and C. PROVIDÊNCIA. "FINITE TEMPERATURE EQUATIONS OF STATE FOR MIXED STARS." International Journal of Modern Physics D 13, no. 07 (August 2004): 1249–53. http://dx.doi.org/10.1142/s0218271804005389.

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We investigate the properties of mixed stars formed by hadronic and quark matter in β-equilibrium described by appropriate equations of state (EOS) in the framework of relativistic mean-field theory. The calculations were performed for T=0 and for finite temperatures and also for fixed entropies with and without neutrino trapping in order to describe neutron and proto-neutron stars. The star properties are discussed. Maximum allowed masses for proto-neutron stars are much larger when neutrino trapping is imposed.
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JAIKUMAR, P., C. GALE, D. PAGE, and M. PRAKASH. "DISTINGUISHING BARE QUARK STARS FROM NEUTRON STARS." International Journal of Modern Physics A 19, no. 31 (December 20, 2004): 5335–42. http://dx.doi.org/10.1142/s0217751x04022566.

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Observations to date cannot distinguish neutron stars from self-bound bare quark stars on the basis of their gross physical properties such as their masses and radii alone. However, their surface luminosity and spectral characteristics can be significantly different. Unlike a normal neutron star, a bare quark star can emit photons from its surface at super-Eddington luminosities for an extended period of time. We present a calculation of the photon bremsstrahlung rate from the bare quark star's surface, and indicate improvements that are required for a complete characterization of the spectrum. The observation of this distinctive photon spectrum would constitute an unmistakable signature of a strange quark star and shed light on color superconductivity at stellar densities.
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Husain, Wasif, Theo F. Motta, and Anthony W. Thomas. "Consequences of neutron decay inside neutron stars." Journal of Cosmology and Astroparticle Physics 2022, no. 10 (October 1, 2022): 028. http://dx.doi.org/10.1088/1475-7516/2022/10/028.

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Abstract The hypothesis that neutrons might decay into dark matter is explored using neutron stars as a testing ground. It is found that in order to obtain stars with masses at the upper end of those observed, the dark matter must experience a relatively strong self-interaction. Conservation of baryon number and energy then require that the star must undergo some heating, with a decrease in radius, leading to an increase in speed of rotation over a period of days.
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Astashenok, A. V., S. Capozziello, S. D. Odintsov, and V. K. Oikonomou. "Maximum baryon masses for static neutron stars in f(R) gravity." Europhysics Letters 136, no. 5 (December 1, 2021): 59001. http://dx.doi.org/10.1209/0295-5075/ac3d6c.

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Abstract We investigate the upper mass limit predictions of the baryonic mass for static neutron stars in the context of f(R) gravity. We use the most popular f(R) gravity model, namely the R 2 gravity, and calculate the maximum baryon mass of static neutron stars adopting several realistic equations of state and one ideal equation of state, namely that of causal limit. Our motivation is based on the fact that neutron stars with baryon masses larger than the maximum mass for static neutron star configurations inevitably collapse to black holes. Thus with our analysis, we want further to enlighten the predictions for the maximum baryon masses of static neutron stars in R 2 gravity, which, in turn, further strengthens our understanding of the mysterious mass gap region. As we show, the baryon masses of most of the equations of states studied in this paper lie in the lower limits of the mass gap region – , but intriguingly enough, the highest value of the maximum baryon masses we found is of the order of . This upper mass limit also appears as a maximum static neutron star gravitational mass limit in other contexts. Combining the two results which refer to baryon and gravitational masses, we point out that the gravitational mass of static neutron stars cannot be larger than three solar masses, while based on maximum baryon masses results of the present work, we can conspicuously state that it is highly likely the lower mass limits of astrophysical black holes in the range of – . This, in turn, implies that maximum neutron star masses in the context of R 2 gravity are likely to be in the lower limits of the range of – . Hence our work further supports the General Relativity claim that neutron stars cannot have gravitational masses larger than and then, to explain observations comparable or over this limit, we need alternative extensions of General Relativity, other than f(R) gravity.
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Heiselberg, Henning, and Vijay Pandharipande. "Recent Progress in Neutron Star Theory." Annual Review of Nuclear and Particle Science 50, no. 1 (December 2000): 481–524. http://dx.doi.org/10.1146/annurev.nucl.50.1.481.

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▪ Abstract We review recent progress in the theory of neutron stars and compare its predictions with the observational data on masses, radii, and temperatures. The theory of neutron stars made up of neutrons, protons, and leptons is discussed in detail along with recent models of nuclear forces and modern many-body techniques. The possibilities of pion and kaon condensation in dense neutron star matter are considered, as is the possible occurrence of strange hyperons and quark-matter drops in the stellar core. The structure of mixed-phase matter in neutron stars, as well as the probable effect of phase transitions on the spin down of pulsars, is also discussed.
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Gondek, Dorota. "Neutron stars and strange stars." International Astronomical Union Colloquium 160 (1996): 133–34. http://dx.doi.org/10.1017/s0252921100041282.

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If strange quark plasma is the real ground state of baryonic matter (Witten 1984), then some of neutron stars (NS) could actually be strange stars (SS). It is difficult to distinguish SS from NS observationally. They have similar radii and masses and their crusts are built of the same matter. It seems that a good method for testing the existence of SS would be the studies of phenomena related to the stellar pulsations. In 1976 Boriakoff proposed that radial oscillations of NS could be observed within radio subpulses of pulsars. While various modes of pulsations of NS were studied by a number of authors, little attention was paid to seismological signatures of SS. The radial oscilations of bare SS were studied by Väth & Chanmugam (1992). Recently Weber (this volume) studied properties of stars made of matter described by BPS equation of state (EOS) (Baym et al. 1971) with a ball of strange matter inside, but they mainly concentrated on stability of white-dwarf-like SS. In this work I present fully relativistic calculations of the radial oscillation frequencies of SS. I determined the fundamental frequency for bare SS and SS with two different types of crusts depending on origin (Alcock et al. 1986) of SS and showed differences between them.
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Dissertations / Theses on the topic "Neutron stars masses"

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Ash, Timothy David Curtis. "The masses of the neutron stars in Cen X-3 and Vela X-1." Thesis, Open University, 1999. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.310006.

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Güver, Tolga, Feryal Özel, Herman Marshall, Dimitrios Psaltis, Matteo Guainazzi, and Maria Díaz-Trigo. "SYSTEMATIC UNCERTAINTIES IN THE SPECTROSCOPIC MEASUREMENTS OF NEUTRON STAR MASSES AND RADII FROM THERMONUCLEAR X-RAY BURSTS. III. ABSOLUTE FLUX CALIBRATION." IOP PUBLISHING LTD, 2016. http://hdl.handle.net/10150/621974.

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Many techniques for measuring neutron star radii rely on absolute flux measurements in the X-rays. As a result, one of the fundamental uncertainties in these spectroscopic measurements arises from the absolute flux calibrations of the detectors being used. Using the stable X-ray burster, GS 1826-238, and its simultaneous observations by Chandra HETG/ACIS-S and RXTE/PCA as well as by XMM-Newton EPIC-pn and RXTE/PCA, we quantify the degree of uncertainty in the flux calibration by assessing the differences between the measured fluxes during bursts. We find that the RXTE/PCA and the Chandra gratings measurements agree with each other within their formal uncertainties, increasing our confidence in these flux measurements. In contrast, XMM-Newton EPIC-pn measures 14.0 +/- 0.3% less flux than the RXTE/PCA. This is consistent with the previously reported discrepancy with the flux measurements of EPIC-pn, compared with EPIC MOS1, MOS2, and ACIS-S detectors. We also show that any intrinsic time-dependent systematic uncertainty that may exist in the calibration of the satellites has already been implicity taken into account in the neutron star radius measurements.
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MONTOLI, ALESSANDRO. "CONSTRAINTS ON NEUTRON STAR STRUCTURE FROM PULSAR GLITCHES." Doctoral thesis, Università degli Studi di Milano, 2020. http://hdl.handle.net/2434/797319.

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Neutron stars are among the densest objects in the Universe, making them a perfect laboratory to study nuclear matter under extreme conditions. Pulsars – rapidly rotating magnetised neutron stars – are one of their possible manifestations, being observed as an extremely regular periodic emission in the radio spectrum. This radiation is produced by converting their rotational energy and, because of this, pulsars are expected to spin down. Some of them, however, have been observed exhibiting sudden accelerations in their rotation, also known as glitches. Nowadays, pulsar glitches are interpreted as the manifestation of vortex dynamics in the internal neutron superfluid, which lags behind the observable charged component in spinning down, occasionally releasing angular momentum to it and giving rise to a glitch. In this work, we will present three different observational characteristics of a glitching pulsar – its largest glitch, its average acceleration due to glitches and its short-time evolution after a glitch – and we will try to extract information about the neutron star from each of them. In particular, we will try to set constraints on the mass of the star, the moment of inertia of its reservoir component and several other quantities tied to the glitch phenomenon, with the ultimate goal of increasing our knowledge about the properties of matter at densities above those of terrestrial nuclei.
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Peralta, Carlos Andrés. "Superfluid spherical Couette flow and rotational irregularities in pulsars /." Connect to thesis, 2006. http://eprints.unimelb.edu.au/archive/00003176.

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Lima, Rodolfo Valentim da Costa. "Análise Bayesiana de dois problemas em Astrofísica Relativística: neutrinos do colapso gravitacional e massas das estrelas de nêutrons." Universidade de São Paulo, 2012. http://www.teses.usp.br/teses/disponiveis/14/14131/tde-26062013-162012/.

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O evento estraordinário de SN1987A vem sendo investigado há mais de vinte e cinco anos. O fascínio que cerca tal evento astronômico está relacionado com a observação em tempo real da explosão à luz da Física de neutrinos. Detectores espalhados pelo mundo observaram um surto neutrinos que dias mais tarde foi confirmado como sendo a SN1987A. Kamiokande, IMB e Baksan apresentaram os eventos detectados que permitiu o estudo de modelos para a explosão e resfriamento da hipotética estrela de nêutrons remanescente. Até hoje não há um consenso a origem do progenitor e a natureza do objeto compacto remanescente. O trabalho se divide em duas partes: estudo dos neutrinos de SN1987A através de Análise Estatística Bayesiana através de um modelo proposto com duas temperaturas que evidenciam dois surtos de neutrinos. A motivação está na hipótese do segundo surto como resultado da formação de matéria estranha no objeto compacto. A metodologia empregada foi a desenvolvida por um trabalho interessante de Loredo (2002) que permite modelar e testar hipóteses sobre os modelos via Bayesian Information Criterion (BIC). A segunda parte do trabalho, a mesma metodologia estatística é usada no estudo da distribuição de massas das estrelas de nêutrons usando a base de dados disponível (http://stellarcollapse.org). A base de dados foi analisada utilizando somente o valor do objeto e seu desvio padrão. Construindo uma função de verossimilhança e utilizando distribuições ``a priori\'\' com hipótese de bimodalidade da distribuição das massas contra uma distribuição unimodal sobre todas as massas dos objetos. O teste BIC indica forte tendência favorável à existência da bimodalidade com valores centrados em 1.37M para objetos de baixa massa e 1.73M para objetos de alta massa e a confirmação da fraca evidência de um terceiro pico esperado em 1.25M.
The extraordinary event of supernova has been investigated twenty five years ago. The fascination surrounds such astronomical event is on the real time observation the explosion at light to neutrino Physics. Detectors spread for the world had observed one burst neutrinos that days later it was confirmed as being of SN1987A. Kamiokande, IMB and Baksan had presented the detected events that allowed to the study of models for the explosion and cooling of hypothetical neutron star remain. Until today it does not have a consensus the origin of the progenitor and the nature of the remaining compact object. The work is divided in two parts: study of the neutrinos of SN1987A through Analysis Bayesiana Statistics through a model considered with two temperatures that two evidence bursts of neutrinos. The motivation is in the hypothesis of as burst as resulted of the formation of strange matter in the compact object. The employed methodology was developed for an interesting work of Loredo & Lamb (2002) that it allows shape and to test hypotheses on the models saw Bayesian Information Criterion (BIC). The second part of the work, the same methodology statistics is used in the study of the distribution of masses of the neutron stars using the available database http://stellarcollapse.org/. The database was analyzed only using the value of the object and its shunting line standard. Constructing to a a priori function likelihood and using distributions with hypothesis of bimodal distribution of the masses against a unimodal distribution on all the masses of objects. Test BIC indicates fort favorable trend the existence of the bimodality with values centered in 1.37M for objects of low mass and 1.73M for objects of high mass and week evidence of one third peak around 1.25M.
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Seveso, S. L. "ADVANCES IN MODELS OF PULSAR GLITCHES." Doctoral thesis, Università degli Studi di Milano, 2015. http://hdl.handle.net/2434/255803.

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Neutron stars are surely one of the most interesting astronomical objects: in no other place of the observable universe, in fact, matter is so compressed that the density reaches and overcomes the nuclear saturation value. This is a so extreme condition that in no terrestrial laboratory we can directly reproduce it in order to study its properties. Neutron stars are therefore a very fascinating research field that can bring us to a deeper understanding of this exotic matter, by modeling the observations of peculiar phenomena related to these stars. This thesis is focused on the pulsar glitches, which are rapid jumps in the rotational velocity of the star. Shortly after the first glitches were observed it was suggested that they could be due to a superfluid component in the stellar interior that could store angular momentum thanks to the pinning interaction between superfluid vortexes and crustal lattice. This qualitative idea suggests that the problem must be faced by merging results which come from the microphysics point of view into a more macroscopic simulation. In this thesis we deal with the evaluation of the vortex--nuclei interaction from the mesoscopic point of view: we perform a realistic calculation of the pinning force per unit length for the inner crust of a neutron star. We find that this mesoscopic interaction is $\approx10^{15} \mbox{ dyn/cm}$, much smaller than previous calculations but still enough to explain glitches. A similar approach has been adopted also in the calculation of the pinning force in the core: if protons in the interior are in a type II superconducting state, an interaction between magnetic flux tubes and rotational vortexes is possible and must be estimated (in case of type I superconductivity the interactions are much weaker). Our results indicate that even in this case, the interaction between vortexes and flux tubes will be significantly weaker than in the crust, as the force per unit length is $\approx 10^{12} - 10^{13} \mbox{ dyn/cm}$. These results are used in static models (based on the "snowplow" model) which can reproduce the physical observable parameters and also provide a mean to infer the masses of the most frequent glitching stars: we propose a unified description of the glitch phenomenon both for small and large glitchers and we analyze the interesting correlation between mass and glitching strength. The whole temporal evolution of a glitch can be followed thanks to the development of a dynamical model. The multifluids formalism is implemented in a consistent simulation, which take into account realistic physical inputs like equation of state, entrainment and drag forces: the rise and the recovery of a glitch is analyzed in connection with the relevant parameters of the model, in order to understand more deeply all the aspects of this phenomenon. We also compare our simulations with the observational data of the frequent glitchers in order to estimate the masses of the pulsars. It's noteworthy the fact that the results are in good agreement with the ones obtained with the static approach, showing again the same mass--glitching strength relation.
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Bhalerao, Varun B. "Neutron Stars and NuSTAR: A Systematic Survey of Neutron Star Masses in High Mass X-ray Binaries & Characterization of CdZnTe Detectors for NuSTAR." Thesis, 2012. https://thesis.library.caltech.edu/7110/1/Bhalerao-V-B-thesis.pdf.

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My thesis centers around the study of neutron stars, especially those in massive binary systems. To this end, it has two distinct components: the observational study of neutron stars in massive binaries with a goal of measuring neutron star masses and participation in NuSTAR, the first imaging hard X-ray mission, one that is extremely well suited to the study of massive binaries and compact objects in our Galaxy.

The Nuclear Spectroscopic Telescope Array (NuSTAR) is a NASA Small Explorer mission that will carry the first focusing high energy X-ray telescope to orbit. NuSTAR has an order-of-magnitude better angular resolution and has two orders of magnitude higher sensitivity than any currently orbiting hard X-ray telescope. I worked to develop, calibrate, and test CdZnTe detectors for NuSTAR. I describe the CdZnTe detectors in comprehensive detail here — from readout procedures to data analysis. Detailed calibration of detectors is necessary for analyzing astrophysical source data obtained by the NuSTAR. I discuss the design and implementation of an automated setup for calibrating flight detectors, followed by calibration procedures and results.

Neutron stars are an excellent probe of fundamental physics. The maximum mass of a neutron star can put stringent constraints on the equation of state of matter at extreme pressures and densities. From an astrophysical perspective, there are several open questions in our understanding of neutron stars. What are the birth masses of neutron stars? How do they change in binary evolution? Are there multiple mechanisms for the formation of neutron stars? Measuring masses of neutron stars helps answer these questions. Neutron stars in high-mass X-ray binaries have masses close to their birth mass, providing an opportunity to disentangle the role of "nature" and "nurture" in the observed mass distributions. In 2006, masses had been measured for only six such objects, but this small sample showed the greatest diversity in masses among all classes of neutron star binaries. Intrigued by this diversity — which points to diverse birth masses — we undertook a systematic survey to measure the masses of neutron stars in nine high-mass X-ray binaries. In this thesis, I present results from this ongoing project.

While neutron stars formed the primary focus of my work, I also explored other topics in compact objects. Appendix A describes the discovery and complete characterization of a 1RXS J173006.4+033813, a polar cataclysmic variable. Appendix B describes the discovery of a diamond planet orbiting a millisecond pulsar, and our search for its optical counterpart.

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Books on the topic "Neutron stars masses"

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Braude, S. Ya, and V. M. Kontorovich. Radio Waves Tell About the Universe. PH “Akademperiodyka”, 2005. http://dx.doi.org/10.15407/akademperiodyka.005.279.

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The book tells about the achievements of modern radio astronomy. Data on radio galaxies, quasars, pulsars, space masers, and other space objects emitting radio waves are presented in a popular form. The ways of evolution of stars, supernovae and radio eruptions of their remains, the formation of white dwarfs and neutron stars, the phenomena in the centers of galaxies and the fusion of galaxies responsible for the formation of radio galaxies and quasars are considered. The radio radiation of the Sun and planets is discussed. A modern view of the evolution of the universe, the origin of the relic radiation left over from the Great Eruption, and its anisotropy is presented. A separate chapter is devoted to the description of radio telescopes.
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Book chapters on the topic "Neutron stars masses"

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Horvath, Jorge E., and Rodolfo Valentim. "The Masses of Neutron Stars." In Handbook of Supernovae, 1–14. Cham: Springer International Publishing, 2016. http://dx.doi.org/10.1007/978-3-319-20794-0_67-1.

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Horvath, Jorge E., and Rodolfo Valentim. "The Masses of Neutron Stars." In Handbook of Supernovae, 1317–30. Cham: Springer International Publishing, 2017. http://dx.doi.org/10.1007/978-3-319-21846-5_67.

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Deich, W. T. S., and S. R. Kulkarni. "The Masses of the Neutron Stars in M15C." In Compact Stars in Binaries, 279–85. Dordrecht: Springer Netherlands, 1996. http://dx.doi.org/10.1007/978-94-009-0167-4_24.

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Popov, Sergei, David Blaschke, Hovik Grigorian, and Mikhail Prokhorov. "Neutron star masses: dwarfs, giants and neighbors." In Isolated Neutron Stars: From the Surface to the Interior, 381–85. Dordrecht: Springer Netherlands, 2007. http://dx.doi.org/10.1007/978-1-4020-5998-8_47.

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Wiescher, M., V. Barnard, J. L. Fisker, J. Görres, K. Langanke, G. Martinez-Pinedo, F. Rembges, H. Schatz, and F. K. Thielemann. "Nuclear-reaction rates in the thermonuclear runaway phase of accreting neutron stars." In Exotic Nuclei and Atomic Masses, 99–103. Berlin, Heidelberg: Springer Berlin Heidelberg, 2003. http://dx.doi.org/10.1007/978-3-642-55560-2_32.

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Picchio, G., M. Busso, and R. Gallino. "The ‘S’ Process Nucleosynthesis in Low Mass Stars and the Neutron Source 13C (α, n) 16O." In Mass Outflows from Stars and Galactic Nuclei, 279–83. Dordrecht: Springer Netherlands, 1988. http://dx.doi.org/10.1007/978-94-009-2941-8_33.

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Aglietta, M., G. Badino, G. Bologna, C. Castagnoli, A. Castellina, V. L. Dadykin, W. Fulgione, et al. "Neutrino Outflow from Supernova 1987A Detected in the Mont Blanc Observatory." In Mass Outflows from Stars and Galactic Nuclei, 367–72. Dordrecht: Springer Netherlands, 1988. http://dx.doi.org/10.1007/978-94-009-2941-8_54.

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"I: Models of rotating relativistic neutron stars of selected masses." In Series in High Energy Physics, Cosmology and Gravitation, 643–48. Bristol and Philadelphia: Institute of Physics Publishing, 2017. http://dx.doi.org/10.1201/9780203741719-29.

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Ostlie, Dale A. "The End of a Stellar Life." In Astronomy: The Human Quest for Understanding, 684–725. Oxford University PressOxford, 2022. http://dx.doi.org/10.1093/oso/9780198825821.003.0017.

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Abstract The End of a Stellar Life considers the consequences of a star that expends all its available fuel. Stars less than about 9 solar masses will grow so large and become so luminous that their very extended atmospheres will gently blow off into space, temporarily forming beautiful planetary nebulas while leaving behind their burned-out nuclear cores. These Earth-sized cinders are known as white dwarfs. If a white dwarf happens to be in a binary star system, material from its companion could fall onto it, pushing its mass above the 1.4 solar mass Chandrasekhar limit, thus triggering a supernova explosion that destroys the star. For more massive stars, the nuclear reactions ultimately lead to collapsing cores and a different sort of supernova. What is left behind is either a bizarre, city-sized neutron star or, if the star’s original mass was large enough, a black hole.
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Moffat, John W. "Early Observations of Black Holes." In The Shadow of the Black Hole, 58–71. Oxford University Press, 2020. http://dx.doi.org/10.1093/oso/9780190650728.003.0004.

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Early observations of black holes, before the LIGO/Virgo detection of gravitational waves, were made by observing electromagnetic processes involving atomic spectral lines. X-ray binary systems were observed consisting of a progenitor star such as a neutron star and a dark companion. X-rays emitted from the gas accreting the dark companion tells us whether it is a black hole. Evidence indicated supermassive black holes at the centers of galaxies. From observations of orbits of stars near the supermassive black holes, one could determine their masses, which proved they were black holes. Observations of quasars, among the brightest objects in the universe, showed they contain black holes. It is important to establish the existence of an event horizon with the black hole, as predicted by general relativity. The current evidence for the event horizon is circumstantial, based on controversial theoretical models about the accretion disks surrounding the collapsed dark objects.
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Conference papers on the topic "Neutron stars masses"

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Nice, David J., Ingrid H. Stairs, Laura E. Kasian, C. Bassa, Z. Wang, A. Cumming, and V. M. Kaspi. "Masses of Neutron Stars in Binary Pulsar Systems." In 40 YEARS OF PULSARS: Millisecond Pulsars, Magnetars and More. AIP, 2008. http://dx.doi.org/10.1063/1.2900273.

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Kızıltan, Bülent, Ersin Göğüş, Ünal Ertan, and Tomaso Belloni. "Reassessing The Fundamentals New Constraints on the Evolution, Ages and Masses of Neutron Stars." In ASTROPHYSICS OF NEUTRON STARS 2010: A Conference in Honor of M. Ali Alpar. AIP, 2011. http://dx.doi.org/10.1063/1.3629483.

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Canalizo, Gabriela, Margrethe Wold, Mariana Lazarova, Mark Lacy, Sandip K. Chakrabarti, and Archan S. Majumdar. "Quasar Black Hole Masses from Velocity Dispersions." In OBSERVATIONAL EVIDENCE FOR BLACK HOLES IN THE UNIVERSE: Proceedings of the 2nd Kolkata Conference on Observational Evidence for Black Holes in the Universe held in Kolkata India, 10–15 February 2008 and the Satellite Meeting on Black Holes, Neutron Stars, and Gamma-Ray Bursts held 16–17 February 2008. AIP, 2008. http://dx.doi.org/10.1063/1.3009525.

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Soria, Roberto, Zdenka Kuncic, Sandip K. Chakrabarti, and Archan S. Majumdar. "Black hole masses and accretion states in ULXs." In OBSERVATIONAL EVIDENCE FOR BLACK HOLES IN THE UNIVERSE: Proceedings of the 2nd Kolkata Conference on Observational Evidence for Black Holes in the Universe held in Kolkata India, 10–15 February 2008 and the Satellite Meeting on Black Holes, Neutron Stars, and Gamma-Ray Bursts held 16–17 February 2008. AIP, 2008. http://dx.doi.org/10.1063/1.3009467.

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Lattimer, James M. "Neutron star masses and radii." In XIAMEN-CUSTIPEN WORKSHOP ON THE EQUATION OF STATE OF DENSE NEUTRON-RICH MATTER IN THE ERA OF GRAVITATIONAL WAVE ASTRONOMY. AIP Publishing, 2019. http://dx.doi.org/10.1063/1.5117791.

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YAKOVLEV, D. G. "MEASUREMENTS OF NEUTRON STAR MASSES." In Proceedings of the International Symposium EXOCT07. WORLD SCIENTIFIC, 2008. http://dx.doi.org/10.1142/9789812797049_0029.

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Lamb, Frederick K., M. Coleman Miller, and Dimitrios Psaltis. "Constraints on neutron star masses and radii from kilohertz QPOs." In Accretion processes in astrophysical systems: Some like it hot! - eigth astrophysics conference. AIP, 1998. http://dx.doi.org/10.1063/1.55923.

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Steiner, Andrew, Tobias Fischer, Stefano Gandolfi, and M. Hempel. "Constraining the Dense Matter from Neutron Star Masses and Radii." In XII International Symposium on Nuclei in the Cosmos. Trieste, Italy: Sissa Medialab, 2013. http://dx.doi.org/10.22323/1.146.0038.

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Miller, M. Coleman, Stratos Boutloukos, Ka Ho Lo, and Frederick K. Lamb. "Implications of high-precision spectra of thermonuclear X-ray bursts for determining neutron star masses and radii." In Fast X-ray timing and spectroscopy at extreme count rates. Trieste, Italy: Sissa Medialab, 2011. http://dx.doi.org/10.22323/1.122.0024.

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