Neutron Stars Formation and Core Collapse Supernovae

Cerda-Duran, Pablo; Elias-Rosa, Nancy

doi:10.1007/978-3-319-97616-7_1

Pablo Cerda-Duran⁷ &
Nancy Elias-Rosa⁸

Part of the book series: Astrophysics and Space Science Library ((ASSL,volume 457))

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Abstract

In the last decade there has been a remarkable increase in our knowledge about core-collapse supernovae (CC-SNe), and the birthplace of neutron stars, from both the observational and the theoretical point of view. Since the 1930s, with the first systematic supernova search, the techniques for discovering and studying extragalactic SNe have improved. Many SNe have been observed, and some of them, have been followed through efficiently and with detail. Furthermore, there has been a significant progress in the theoretical modelling of the scenario, boosted by the arrival of new generations of supercomputers that have allowed to perform multidimensional numerical simulations with unprecedented detail and realism. The joint work of observational and theoretical studies of individual SNe over the whole range of the electromagnetic spectrum has allowed to derive physical parameters, which constrain the nature of the progenitor, and the composition and structure of the star’s envelope at the time of the explosion. The observed properties of a CC-SN are an imprint of the physical parameters of the explosion such as mass of the ejecta, kinetic energy of the explosion, the mass loss rate, or the structure of the star before the explosion. In this chapter, we review the current status of SNe observations and theoretical modelling, the connection with their progenitor stars, and the properties of the neutron stars left behind.

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Notes

1.
http://www.darkenergysurvey.org/.
2.
This distance limit is based on practical experience. Smartt et al. (2009) and Eldridge et al. (2013) set to 28 Mpc the distance limit for a feasible search of SN progenitors, although there are exceptions such as the massive progenitor of SN 2005gl at 60 Mpc (Gal-Yam et al. 2007).
3.
Note however that pop III stars have very massive (M > 100M _⊙) iron cores with high entropy (s ∼ 8k _B per baryon) and may form black holes promptly (Sekiguchi and Shibata 2011).
4.
The reader should not confuse the parameter ξ _2.5 with the compactness of a neutron star (M _NS∕R _NS) often appearing in the literature, despite of its similarity in name and definition. While more compact neutron stars have higher values of M _NS∕R _NS, a higher value of ξ _2.5 indicates that the core of the star is more extended (less compact).

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Acknowledgements

This work is supported by the New Compstar COST action MP1304. N.E.R. acknowledges financial support by the 1994 PRIN-INAF 2014 (project ‘Transient Universe: unveiling new types of stellar explosions with PESSTO’). N.E.R. acknowledges the hospitality of the “Institut de Ciències de l’Espai” (CSIC), where part of this work has been done. P.C.D. acknowledges the financial support from the Spanish Ministerio de Economía y Competitividad (grant AYA2015-66899-C2-1-P) and from the Generalitat Valenciana (grant PROMETEO-II-2014-069).

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Departamento de Astronomía y Astrofísica, Universitat de València, Valencia, Spain
Pablo Cerda-Duran
INAF - Osservatorio Astronomico di Padova, Padova, Italy
Nancy Elias-Rosa

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Institut für Theoretische Physik, Goethe University Frankfurt, Frankfurt, Hessen, Germany
Luciano Rezzolla
Dipartimento di Fisica, Universita’ degli Studi di Milano, Milan, Italy
Pierre Pizzochero
Mathematical Sciences, University of Southampton, Southampton, UK
David Ian Jones
Institute of Space Sciences (ICE), Consejo Superior de Investigaciones Científicas (CSIC), Barcelona, Spain
Nanda Rea
Istituto Nazionale di Fisica Nucleare (INFN), Dipartimento di Fisica, Università di Catania, Catania, Italy
Isaac Vidaña

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Cerda-Duran, P., Elias-Rosa, N. (2018). Neutron Stars Formation and Core Collapse Supernovae. In: Rezzolla, L., Pizzochero, P., Jones, D., Rea, N., Vidaña, I. (eds) The Physics and Astrophysics of Neutron Stars. Astrophysics and Space Science Library, vol 457. Springer, Cham. https://doi.org/10.1007/978-3-319-97616-7_1

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Print ISBN: 978-3-319-97615-0
Online ISBN: 978-3-319-97616-7
eBook Packages: Physics and AstronomyPhysics and Astronomy (R0)

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