Relevant bibliographies by topics / Neutron stars

Academic literature on the topic 'Neutron stars'

Author: Grafiati
Published: 4 June 2021
Last updated: 29 July 2024

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Journal articles on the topic "Neutron stars"

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Wang, Zhen-Ru. "Ancient Guest Stars as Harbingers of Neutron Star Formation." Symposium - International Astronomical Union 125 (1987): 305–18. http://dx.doi.org/10.1017/s0074180900160917.

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It was just after the discovery of neutrons in 1932, Landau suggested the possibility of compact stars composed of neutrons. In 1934 Baade and Zwicky proposed the idea of neutron stars independently and suggested that neutron stars would be formed in supernova explosions.
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Woltjer, L. "Where Neutron Stars Come From, How Neutron Stars Evolve, and Neutron Stars Go." Symposium - International Astronomical Union 125 (1987): 559–62. http://dx.doi.org/10.1017/s007418090016142x.

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Yakovlev, D. "Neutrino emission from neutron stars." Physics Reports 354, no. 1-2 (November 2001): 1–155. http://dx.doi.org/10.1016/s0370-1573(00)00131-9.

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Kolomeitsev, E. E., and D. N. Voskresensky. "Neutrino Processes in Neutron Stars." EPJ Web of Conferences 7 (2010): 03003. http://dx.doi.org/10.1051/epjconf/20100703003.

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Seward, F. "Neutron Stars." Science 262, no. 5132 (October 15, 1993): 444–45. http://dx.doi.org/10.1126/science.262.5132.444.

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Vartanyan, Yu L., and G. B. Alaverdyan. "Neutron stars." Astrophysics 31, no. 1 (1990): 482–89. http://dx.doi.org/10.1007/bf01004395.

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Ho, Wynn C. G., Craig O. Heinke, Daniel J. Patnaude, Peter S. Shternin, and Dmitry G. Yakovlev. "Hottest Superfluid and Superconductor in the Universe: Lessons from the Cooling of the Cassiopeia A Neutron Star." Proceedings of the International Astronomical Union 7, S285 (September 2011): 337–39. http://dx.doi.org/10.1017/s1743921312000981.

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AbstractThe cooling rate of young neutron stars gives direct insight into their internal makeup. Using Chandra observations of the 330-year-old Cassiopeia A supernova remnant, we find that the temperature of the youngest-known neutron star in the Galaxy has declined by 4% over the last 10 years. The decline is explained naturally by superconductivity and superfluidity of the protons and neutrons in the stellar core. The protons became superconducting early in the life of the star and suppressed the early cooling rate; the neutron star thus remained hot before the (recent) onset of neutron superfluidity. Once the neutrons became superfluid, the Cooper pair-formation process produced a splash of neutrino emission which accelerated the cooling and resulted in the observed rapid temperature decline. This is the first time a young neutron star has been seen to cool in real time, and is the first direct evidence, from cooling observations, of superfluidity and superconductivity in the core of neutron stars.
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Yakovlev, D. G. "Non-equilibrium neutron stars." International Journal of Modern Physics A 35, no. 02n03 (January 30, 2020): 2040049. http://dx.doi.org/10.1142/s0217751x20400497.

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Neutron stars contain superdense matter in their interiors. Characteristic densities in their cores are several times higher than the standard density of nuclear matter. This matter is so dense that it would be natural to assume that frequent particle collisions produce immediate equilibration. However, because of the slowness of some reactions, the equilibration with respect to them can be greatly delayed. Then one should deal with non-equilibrium stars which contain extra energy to be released. Deviations from equilibrium can affect neutrino emission of neutron stars, warm up their interiors and influence their thermal evolution. The effects of equilibration can be important for pulsating, rotating, accreting neutron stars, as well as for merging binary neutron stars.
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Chakraborty, Sabyasachi, Aritra Gupta, and Miguel Vanvlasselaer. "Anomaly induced cooling of neutron stars: a Standard Model contribution." Journal of Cosmology and Astroparticle Physics 2023, no. 10 (October 1, 2023): 030. http://dx.doi.org/10.1088/1475-7516/2023/10/030.

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Abstract Young neutron stars cool via the emission of neutrinos from their core. A precise understanding of all the different processes producing neutrinos in the hot and degenerate matter is essential for assessing the cooling rate of such stars. The main Standard Model processes contributing to this effect are ν bremsstrahlung, mURCA among others. In this paper, we investigate another Standard Model process initiated by the Wess-Zumino-Witten term, leading to the emission of neutrino pairs via Nγ → Nνν̅. We find that for proto-neutron stars, such processes with degenerate neutrons can be comparable and even dominate over the typical and well-known cooling mechanisms.
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Noda, Tsuneo, Nobutoshi Yasutake, Masa-aki Hashimoto, Toshiki Maruyama, and Toshitaka Tatsumi. "Cooling of neutron stars with quark-hadron continuity." EPJ Web of Conferences 260 (2022): 11024. http://dx.doi.org/10.1051/epjconf/202226011024.

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Neutron stars are high-density objects formed by the gravitational collapse of massive stars, and the whole star can be likened to a giant nucleus. The interior of a neutron star is considered to contain exotic particles and states which do not appear in a normal nucleus. The internal states are constrained by observations of masses and radii via the equation of state of highly dense nuclear matter. Within these constraints, a variety of exotic states have been discussed. The internal state of neutron stars is closely related to its neutrino emission process, which cools the star from the inside. This effect can be compared with observations of the surface temperature of neutron stars. However, despite the wide range of observations of neutron stars, the nature of the neutron star matter remains uncertain. We consider quark matter as an exotic state and perform cooling calculations for neutron stars, incorporating the effects of nucleon superfluidity and quark colour superconductivity.We take into account the “quark-hadron continuity”, in which the neutron superfluidity is succeeded by thedquark pairing. Furthermore, we obtained the range of the neutron star cooling curve, taking into account the difference in surface temperature due to the composition of the surface layer. We found that the existence of quark matter causes strong neutrino emission from quarks, which is moderately suppressedbysuperfluidity and superconductivity, and canexplain the cold surface temperature of neutron stars.
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Dissertations / Theses on the topic "Neutron stars"

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Cernohorsky, Jan. "Neutrino driven neutron star formation." Amsterdam : Amsterdam : Rodopi ; Universiteit van Amsterdam [Host], 1990. http://dare.uva.nl/document/91884.

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Roark, Jacob Brian. "The Deconfinement Phase Transition in Neutron Stars and Proto-Neutron Stars." Kent State University / OhioLINK, 2018. http://rave.ohiolink.edu/etdc/view?acc_num=kent1542979864566784.

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Naso, Luca. "Magnetic Fields in Proto-Neutron Stars and in Accretion Discs Around Neutron Stars." Doctoral thesis, SISSA, 2009. http://hdl.handle.net/20.500.11767/4267.

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Themain characters of this thesis are themagnetic field, the plasma velocity field, the turbulentmagnetic resistivity and the numerical codes. They act on two different stages and on two different levels and occasionaly there are other bit players, e.g. the α-effect, the quenching, the differential rotation, themagnetic streamfunction, themagnetic Reynolds number, the Interactive Data Language and even ZEUS. All of them are led by the same invisible hand with the purpose of understanding better the intricate topic of the magnetic field - plasma relation. The two stages of the scene could not be more different, in one case everything is done in less than a minute inside a proto-neutron star soon after a supernova explosion, in the other case there is no time evolution at all and an equilibrium configuration is looked for inside a disc ofmatter spiraling around a neutron star. Nevertheless the same set of equations can describe the behaviour of the characters on both stages, this set is composed of the equations of the electromagnetic field plus the fluid equations. However knowing that the answers to all of your questions are written inside only one book, does not mean that you are able to read that book ... It is at this moment that the numerical codes come into the scene, offering you a way of translating the book in a language that you know. Unfortunately they like playing tricks and you cannot trust their translations unless you take many precautions every time. Eventually, after the equations have been solved, comes the art of interpreting the results; a task that might seem quite simple in comparison with the difficulties overcome on the path to get there, but that requires a deep knowledge of what has already been done and a good intuition about what can possibly happen later on. We do not presume to have made big leaps forward in the process of understanding the behaviour of the magnetic field in the cases considered here, nonetheless thanks to our simplified models we were able to grasp the fundamental aspects of the phenomena being considered, to gain some insights and to propose new falsifiable ideas. At the same time we have also developed new tools for making our models more elaborate and realistic. Therefore we expect to find even more characters in the future Chapters of this analysis, but that is another story, and will be told another time.
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Riz, Luca. "Spin polarization effects in neutron stars." Doctoral thesis, Università degli studi di Trento, 2020. http://hdl.handle.net/11572/253498.

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This thesis is concerned with effects of spin polarization in neutron stars. In particular, we focus on static and dynamic properties of dense neutron matter. We use two different kind of potential to perform our studies: the phenomenological two-body Argonne V$8$' potential plus the three-body Urbana IX force and a modern local version of chiral effective potential up to next-to-next-to-leading order (N$2$LO). Estimates are calculated for the neutrino mean free path in partially spin-polarized neutron matter starting from Quantum Monte Carlo (QMC) simulations and using mean-field approaches to compute the response function in the longitudinal and transverse channel. We also compute magnetic susceptibility of dense neutron matter from accurate QMC calculations of partially spin-polarized systems. Twist-averaged boundary conditions (TABC) have been implemented to reduce finite-size effects. In the results, we also account for the theoretical uncertainty coming from the chiral expansion scheme. These results may play a role in studying high-energy phenomena such as neutron star mergers and supernova explosions, although they have been computed only at T$=0$ K.
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Riz, Luca. "Spin polarization effects in neutron stars." Doctoral thesis, Università degli studi di Trento, 2020. http://hdl.handle.net/11572/253498.

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This thesis is concerned with effects of spin polarization in neutron stars. In particular, we focus on static and dynamic properties of dense neutron matter. We use two different kind of potential to perform our studies: the phenomenological two-body Argonne V$8$' potential plus the three-body Urbana IX force and a modern local version of chiral effective potential up to next-to-next-to-leading order (N$2$LO). Estimates are calculated for the neutrino mean free path in partially spin-polarized neutron matter starting from Quantum Monte Carlo (QMC) simulations and using mean-field approaches to compute the response function in the longitudinal and transverse channel. We also compute magnetic susceptibility of dense neutron matter from accurate QMC calculations of partially spin-polarized systems. Twist-averaged boundary conditions (TABC) have been implemented to reduce finite-size effects. In the results, we also account for the theoretical uncertainty coming from the chiral expansion scheme. These results may play a role in studying high-energy phenomena such as neutron star mergers and supernova explosions, although they have been computed only at T$=0$ K.
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Tang, Pui-shan Anisia. "The physics of neutron stars." Click to view the E-thesis via HKUTO, 2007. http://sunzi.lib.hku.hk/hkuto/record/B38297036.

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Tang, Pui-shan Anisia, and 鄧珮姗. "The physics of neutron stars." Thesis, The University of Hong Kong (Pokfulam, Hong Kong), 2007. http://hub.hku.hk/bib/B38297036.

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Viganò, Daniele. "Magnetic fields in neutron stars." Doctoral thesis, Universidad de Alicante, 2013. http://hdl.handle.net/10045/36185.

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González, Boquera Claudia. "Neutron-rich matter in atomic nuclei and neutron stars." Doctoral thesis, Universitat de Barcelona, 2020. http://hdl.handle.net/10803/668774.

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The proper understanding of the equation of state (EoS) of highly asymmetric nuclear matter is essential when studying systems such as neutron stars (NSs). Using zero-range Skyrme interactions and finite-range interactions such as Gogny forces, momentum-dependent interactions (MDI) and simple effective interactions (SEI), we analyze the properties of the EoS and the influence they may have on the calculations for NSs. We start by studying the convergence properties of the Taylor series expansion of EoS in powers of the isospin asymmetry. Next, we analyze the accuracy of the results for β-stable nuclear matter, which is found in the interior of NSs, when it is computed using the Taylor expansion of the EoS. The agreement with the results obtained using the full expression of the EoS is better for interactions with small-to-moderate values of the slope of the symmetry energy L. The mass and radius relation for a NS is obtained by integrating the so-called Tolman-Oppenheimer-Volkoff (TOV) equations, where the input is the EoS of the system. We have studied the mass-radius relation for Skyrme and Gogny interactions, and we see that that very soft forces are not able to give stable solutions of the TOV equations and only the stiff enough parametrizations can provide 2M0 NSs. We also notice that none of the existing parametrizations of the standard Gogny D1 interaction is able to provide a NS inside the observational constraints. Because of that, we propose a new parametrization, which we name D1M∗, that is able to provide NSs of 2M0 while still providing the same good description of finite nuclei as D1M. A parametrization D1M∗∗ is also presented, which is fitted in the same way as D1M∗ and provides NSs up to 1.91M0. Moreover, we estimate the core-crust transition in NSs by finding where the nuclear matter in the core is unstable against fluctuations of the density. To do that, we employ two methods, the thermodynamical method and the dynamical method. In the case of finite-range interactions, such as the Gogny ones, to use the dynamical method we have had to derive the explicit expression of the energy curvature matrix in momentum space for this type of interactions. We observe a decreasing trend of the transition density with the slope L of the symmetry energy, while the correlation between the transition pressure and L is much lower. Finally different NS properties are studied. The crustal properties, such as the crustal mass, crustal thickness and crustal fraction of the moment of inertial have lower values if one computes them using the core-crust transition density obtained with the dynamical method instead of the one obtained with the thermodynamical method, pointing out the importance of the accurate evaluation of the transition density when studying observational phenomena. We have also studied the moment of inertia of NSs, which is compared to constraints proposed in the literature. Finally, the tidal deformability for NSs is also calculated and compared with the constraints coming from the GW170817 event detected by the LIGO and Virgo observatories and which accounts for the merger of two NSs in a binary system.
El coneixement de l’equació d’estat (EoS) de matèria altament densa i assimètrica és essencial per tal d’estudiar les estrelles de neutrons (NSs). En aquesta tesi s’analitzen, utilitzant interaccions de camp mig no relativistes, les propietats de l’EoS i la seva influència en càlculs de NSs. Primerament, s’estudia la convergència del desenvolupament en sèrie de Taylor de l’EoS en potències de l'assimetria d’isospí. Seguidament, s’analitza l’exactitud dels resultats per matèria β-estable, la qual es troba a l’interior de les NSs, quan es calcula utilitzant el desenvolupament de Taylor de l’EoS. La relació entre la massa i el radi obtinguda integrant les equacions Tolman-Oppenheimer-Volkoff (TOV) també és estudiada. A causa de que les interaccions de Gogny de la família D1 no aconsegueixen donar NSs compatibles amb observacions astrofísiques, en aquesta tesi proposem dues noves forces de Gogny, anomenades D1M∗ i D1M∗∗, les quals poden donar, respectivament, NSs de 2 i 1.91 masses solars. Una altra part de la tesi es dedica a l’estudi de la transició entre l’escorça i el nucli, buscant la densitat a la qual la matèria uniforme al nucli és inestable contra fluctuacions de densitat. Ho estudiem amb dos mètodes, el mètode termodinàmic i el mètode dinàmic. Finalment, s’analitzen diverses propietats de les NSs, com són la relació entre la massa i el radi de l’estrella, les propietats de l’escorça, el moment d’inèrcia, així com la deformació deguda als corrents de marea (tidal deformability) que està relacionada amb l’emissió d’ones gravitacionals en sistemes binaris d’estrelles de neutrons.
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Thurman, Hugh O. Copeland Gary E. "Neutron star electromagnetic field structure /." Connect to this resource. (Authorized users only), 2004.

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Books on the topic "Neutron stars"

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Y, Potekhin A., and Yakovlev D. G, eds. Neutron stars. New York: Springer, 2006.

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Haensel, P., A. Y. Potekhin, and D. G. Yakovlev, eds. Neutron Stars 1. New York, NY: Springer New York, 2007. http://dx.doi.org/10.1007/978-0-387-47301-7.

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Ögelman, H., and E. P. J. Heuvel, eds. Timing Neutron Stars. Dordrecht: Springer Netherlands, 1989. http://dx.doi.org/10.1007/978-94-009-2273-0.

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H, Ögelman, and Heuvel, Edward Peter Jacobus van den, 1940-, eds. Timing neutron stars. Dordrecht: Kluwer Academic Publishers, 1989.

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Bertulani, Carlos A., and Jorge Piekarewicz. Neutron star crust. Hauppauge, N.Y: Nova Science Publishers, 2011.

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United States. National Aeronautics and Space Administration., ed. Converting neutron stars into strange stars. [Batavia, Ill.?]: Fermi National Accelerator Laboratory, 1991.

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Becker, Werner, ed. Neutron Stars and Pulsars. Berlin, Heidelberg: Springer Berlin Heidelberg, 2009. http://dx.doi.org/10.1007/978-3-540-76965-1.

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Lipunov, Vladimir M. Astrophysics of Neutron Stars. Berlin, Heidelberg: Springer Berlin Heidelberg, 1992. http://dx.doi.org/10.1007/978-3-642-76350-2.

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Paweł, Haensel, Frieman Joshua A, and United States. National Aeronautics and Space Administration., eds. Dibaryons in neutron stars. [Batavia, Ill.]: Fermi National Accelerator Laboratory, 1991.

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M, Kaminker A., ed. Physics of neutron stars. Commack, N.Y: Nova Science Publishers, 1995.

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Book chapters on the topic "Neutron stars"

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Fischer, Daniel, and Hilmar Duerbeck. "Neutron Stars." In Hubble Revisited, 126–27. New York, NY: Springer New York, 1998. http://dx.doi.org/10.1007/978-1-4612-2232-3_19.

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Kippenhahn, Rudolf, Alfred Weigert, and Achim Weiss. "Neutron Stars." In Astronomy and Astrophysics Library, 497–508. Berlin, Heidelberg: Springer Berlin Heidelberg, 2012. http://dx.doi.org/10.1007/978-3-642-30304-3_38.

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Kippenhahn, Rudolf, and Alfred Weigert. "Neutron Stars." In Astronomy and Astrophysics Library, 380–89. Berlin, Heidelberg: Springer Berlin Heidelberg, 1990. http://dx.doi.org/10.1007/978-3-642-61523-8_36.

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Michaud, Georges, Georges Alecian, and Jacques Richer. "Neutron Stars." In Atomic Diffusion in Stars, 259–70. Cham: Springer International Publishing, 2015. http://dx.doi.org/10.1007/978-3-319-19854-5_14.

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Courvoisier, Thierry J. L. "Neutron Stars." In High Energy Astrophysics, 191–203. Berlin, Heidelberg: Springer Berlin Heidelberg, 2012. http://dx.doi.org/10.1007/978-3-642-30970-0_13.

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Keane, Evan Francis. "Neutron Stars." In The Transient Radio Sky, 15–39. Berlin, Heidelberg: Springer Berlin Heidelberg, 2011. http://dx.doi.org/10.1007/978-3-642-19627-0_2.

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Glendenning, Norman K. "Neutron Stars." In Compact Stars, 180–246. New York, NY: Springer US, 1997. http://dx.doi.org/10.1007/978-1-4684-0491-3_5.

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Benhar, Omar, and Stefano Fantoni. "Neutron Stars." In Nuclear Matter Theory, 109–19. Boca Raton: CRC Press, 2020.: CRC Press, 2020. http://dx.doi.org/10.1201/9781351175340-6.

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Feldbaum, David M. "Neutron Stars." In Gravitational Waves: An Overview, 83–84. Cham: Springer International Publishing, 2020. http://dx.doi.org/10.1007/978-3-031-02613-3_15.

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Bandyopadhyay, Debades, and Kamales Kar. "Neutron Stars." In Supernovae, Neutron Star Physics and Nucleosynthesis, 49–133. Cham: Springer International Publishing, 2021. http://dx.doi.org/10.1007/978-3-030-95171-9_3.

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Conference papers on the topic "Neutron stars"

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YAKOVLEV, D. G., M. E. GUSAKOV, A. D. KAMINKER, and A. Y. POTEKHIN. "NEUTRINO EMISSION FROM NEUTRON STARS." In Proceedings of the Carpathian Summer School of Physics 2005. WORLD SCIENTIFIC, 2006. http://dx.doi.org/10.1142/9789812772862_0024.

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Weber, Fridolin. "Neutron stars." In INTERSECTIONS BETWEEN PARTICLE AND NUCLEAR PHYSICS. ASCE, 1997. http://dx.doi.org/10.1063/1.54240.

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Heuvel, Ed van den. "Neutron Stars." In 26th Solvay Conference on Physics: “Astrophysics and Cosmology”. WORLD SCIENTIFIC, 2016. http://dx.doi.org/10.1142/9789814759182_0002.

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WEBER, FRIDOLIN. "NEUTRON STARS AND QUARK STARS." In Proceedings of the KIAS–APCTP International Symposium on Astro-Hadron Physics. WORLD SCIENTIFIC, 2004. http://dx.doi.org/10.1142/9789812702524_0010.

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DEXHEIMER, V., S. SCHRAMM, and H. STOECKER. "PROTO-NEUTRON AND NEUTRON STARS." In Proceedings of the Third Workshop (IWARA07). WORLD SCIENTIFIC, 2010. http://dx.doi.org/10.1142/9789814304887_0004.

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Piekarewicz, J. "Neutron skins and neutron stars." In WORKSHOP TO EXPLORE PHYSICS OPPORTUNITIES WITH INTENSE, POLARIZED ELECTRON BEAMS AT 50-300 MEV. AIP, 2013. http://dx.doi.org/10.1063/1.4829416.

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van der Klis, M. "Timing Neutron Stars." In INTERACTING BINARIES: Accretion, Evolution, and Outcomes. AIP, 2005. http://dx.doi.org/10.1063/1.2130253.

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HOROWITZ, C. J. "NEUTRON RICH NUCLEI AND NEUTRON STARS." In Proceedings of the Fifth International Conference on ICFN5. WORLD SCIENTIFIC, 2013. http://dx.doi.org/10.1142/9789814525435_0065.

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Zhang, Dong, Z. G. Dai, Yong-Feng Huang, Zi-Gao Dai, and Bing Zhang. "Hyperaccreting Neutron Stars and Neutrino-cooled Disks." In 2008 NANJING GAMMA-RAY BURST CONFERENCE. AIP, 2008. http://dx.doi.org/10.1063/1.3027932.

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van den Heuvel, E. P. J. "Double Neutron Stars: Evidence For Two Different Neutron‐Star Formation Mechanisms." In THE MULTICOLORED LANDSCAPE OF COMPACT OBJECTS AND THEIR EXPLOSIVE ORIGINS. American Institute of Physics, 2007. http://dx.doi.org/10.1063/1.2774916.

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Reports on the topic "Neutron stars"

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Christiansen, Michael B., and Norman K. Glendenning. Structured mixed phase is favored in neutron stars. Office of Scientific and Technical Information (OSTI), January 2003. http://dx.doi.org/10.2172/860285.

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Esbensen, H., R. A. Broglia, E. Vigezzi, and F. Barranco. Pairing gap in the inner crust of neutron stars. Office of Scientific and Technical Information (OSTI), August 1995. http://dx.doi.org/10.2172/166474.

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Prakash, M., P. J. Ellis, E. K. Heide, and S. Rudaz. Neutron stars and nuclei in the modified relativistic Hartree approximation. Office of Scientific and Technical Information (OSTI), March 1993. http://dx.doi.org/10.2172/10162477.

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Prakash, M., P. J. Ellis, E. K. Heide, and S. Rudaz. Neutron stars and nuclei in the modified relativistic Hartree approximation. Office of Scientific and Technical Information (OSTI), March 1993. http://dx.doi.org/10.2172/6075573.

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Potekhin, A. Partially Ionized Atmospheres of Neutron Stars with Strong Magnetic Fields. Office of Scientific and Technical Information (OSTI), January 2005. http://dx.doi.org/10.2172/839670.

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Mathews, G. Hydrodynamics and nucleosynthesis in neutron stars, supernovae, and the early universe. Office of Scientific and Technical Information (OSTI), March 1996. http://dx.doi.org/10.2172/278392.

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Tournear, Derek M. Non-Quiescent X-ray Emission from Neutron Stars and Black Holes. Office of Scientific and Technical Information (OSTI), August 2003. http://dx.doi.org/10.2172/815297.

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8

Falato, Michael, Irina Sagert, Oleg Korobkin, and Hyun Lim. Simulating Neutron Stars With Solid Quark Cores: Rotations, Oscillations, and Binary Mergers. Office of Scientific and Technical Information (OSTI), June 2023. http://dx.doi.org/10.2172/1985855.

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9

Hernquist, L. Accretion of matter onto highly magnetized neutron stars: Final report, July 1-September 30, 1985. Office of Scientific and Technical Information (OSTI), June 1986. http://dx.doi.org/10.2172/6067541.

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10

Ajello, M. Limits on Large Extra Dimensions Based on Observations of Neutron Stars with the Fermi-LAT. Office of Scientific and Technical Information (OSTI), August 2012. http://dx.doi.org/10.2172/1049752.

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