Built on

D. Chatterjee and D. Bandyopadhyay, Phys. Rev. D80
Original
1949
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G. Baym, C. Pethick, and P. Sutherland, Astrophys. J. 170
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1981
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J. L. Zdunik, P. Haensel, and R. Schaeffer, Astron. Astrophys. 172
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S. Banik and D. Bandyopadhyay, Phys. Rev. C64
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S. Banik, M. Hanauske, D. Bandyopadhyay, and W. Greiner, Phys. Rev. D70
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2012
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D. E. Alvarez-Castillo and D. Blaschke, in 17th Conference of Young Scientists and Specialists (AYSS ’13) Dubna, Russia, April 8-12, 2013 (2013) arXiv:1304.7758 [astro-ph.HE]
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I. F. Ranea-Sandoval, S. Han, M. G. Orsaria, G. A. Contrera, F. Weber, and M. G. Alford, Phys. Rev. C93
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F. Ozel, D. Psaltis, Z. Arzoumanian, S. Morsink, and M. Baubock, Astrophys. J. 832
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B. Abbott et al. (Virgo, LIGO Scientific), Phys. Rev. Lett. 119
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2018

Can magnetic fields stabilize or destabilize twin stars?

Gomes, R. O., Dexheimer, V., Han, S. et al.

Understand

Sharp phase transitions described by stiff equations of state allow for the existence of a third family of stable compact stars (besides white dwarfs and neutron stars), twin stars.

In this work, we investigate for the first time the role of strong magnetic fields on non-magnetic twin stars sequences and the case in which magnetic fields themselves give rise to a third family of stable stars.
We use three sets of equations of state to study such effects from a more general point of view: the Quark-Hadron Chiral Parity-Doublet (Q$\chi$P) model for both hadronic and quark phases, and the Many-Body Forces (MBF) model connected to either the MIT Bag model with vector interaction (MIT) or to the Constant-Sound-Speed (CSS) approximation for the quark phase, through a Maxwell construction.
Magnetic field effects are introduced in the structure of stars through the solution of the Einstein-Maxwell equations, assuming a poloidal magnetic field configuration and a metric that allows for the description of deformed stars.

Built on

D. Chatterjee and D. Bandyopadhyay, Phys. Rev. D80
Original
1949
Earlier work this paper cites.
U. H. Gerlach, Phys. Rev. 172
1968
Earlier work this paper cites.
G. Baym, C. Pethick, and P. Sutherland, Astrophys. J. 170
1971
Earlier work this paper cites.
J. W. Negele and D. Vautherin, Nucl. Phys. A 207
1973
Earlier work this paper cites.
B. Kampfer, J. Phys. A14
1981
Earlier work this paper cites.
J. L. Zdunik, P. Haensel, and R. Schaeffer, Astron. Astrophys. 172
1987
Earlier work this paper cites.
S. Bonazzola, E. Gourgoulhon, M. Salgado, and J. A. Marck, Astron. Astrophys. 278
1993
Earlier work this paper cites.
N. K. Glendenning and C. Kettner, Astron. Astrophys. 353
2000
Earlier work this paper cites.
K. Schertler, C. Greiner, J. Schaffner-Bielich, and M. H. Thoma, Nucl. Phys. A677
2000
Earlier work this paper cites.
S. Banik and D. Bandyopadhyay, Phys. Rev. C64
2001
Earlier work this paper cites.
S. Banik and D. Bandyopadhyay, Phys. Rev. D67
2003
Earlier work this paper cites.
S. Banik, M. Hanauske, D. Bandyopadhyay, and W. Greiner, Phys. Rev. D70
2004
Earlier work this paper cites.
M. Alford, M. Braby, M. W. Paris, and S. Reddy, Astrophys. J. 629
2005
Earlier work this paper cites.
S. Weissenborn, I. Sagert, G. Pagliara, M. Hempel, and J. Schaffner-Bielich, Astrophys. J. 740
Original
2011
Earlier work this paper cites.
F. Gulminelli, A.-R. Raduta, J. Margueron, P. Papakonstantinou, and M. Oertel, International Summer School for Advanced Studies ’Dynamics of open nuclear systems’
Original
2012
Earlier work this paper cites.
D. E. Alvarez-Castillo and D. Blaschke, in 17th Conference of Young Scientists and Specialists (AYSS ’13) Dubna, Russia, April 8-12, 2013 (2013) arXiv:1304.7758 [astro-ph.HE]
Original
2013
Earlier work this paper cites.