Author

Mandal, Soma

INSPIRE profile1347092 ORCID0000-0002-1047-9911

3 papers·10 citations in this corpus

	Paper	Category
Sep 20, 2005#6*astro-ph/0509538	Neutron Star Equation of State and the Possibility of Complex Self-Energy in Landau Theory of Fermi Liquid in Presence of Strong Quantizing Magnetic Field Soma Mandal🇮🇳 · Roni Saha🇮🇳 · Sutapa Ghosh🇮🇳 · Somenath Chakrabarty🇮🇳	↳ astro-ph	PRC	7
Sep 7, 2004#3*astro-ph/0409109	Chiral Symmetry Breaking in Presence of Strong Quantizing Magnetic Fields- A Nambu-Jona-Lasino Model with Semi-Classical Approximation Sutapa Ghosh🇮🇳 · Soma Mandal🇮🇳 · Somenath Chakrabarty🇮🇳	↳ astro-ph	—	0
May 28, 2002#5*astro-ph/0205445	Impossibility of Spin Polarized States for Neutron Star / Proto-neutron Star Matter in $β$ -Equilibrium Condition Sutapa Ghosh · Soma Mandal · Somenath Chakrabarty	↳ astro-ph	Mod.Phys.Lett.A	3

Neutron Star Equation of State and the Possibility of Complex Self-Energy in Landau Theory of Fermi Liquid in Presence of Strong Quantizing Magnetic Field
Soma Mandal🇮🇳 · Roni Saha🇮🇳 · Sutapa Ghosh🇮🇳 · Somenath Chakrabarty🇮🇳
Sep 20, 2005#6*↳ astro-phPRC7 citations
Chiral Symmetry Breaking in Presence of Strong Quantizing Magnetic Fields- A Nambu-Jona-Lasino Model with Semi-Classical Approximation
Sutapa Ghosh🇮🇳 · Soma Mandal🇮🇳 · Somenath Chakrabarty🇮🇳
Sep 7, 2004#3*↳ astro-ph0 citations
Impossibility of Spin Polarized States for Neutron Star / Proto-neutron Star Matter in $β$ -Equilibrium Condition
Sutapa Ghosh · Soma Mandal · Somenath Chakrabarty
May 28, 2002#5*↳ astro-phMod.Phys.Lett.A3 citations

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Mandal, Soma

Neutron Star Equation of State and the Possibility of Complex Self-Energy in Landau Theory of Fermi Liquid in Presence of Strong Quantizing Magnetic Field

Chiral Symmetry Breaking in Presence of Strong Quantizing Magnetic Fields- A Nambu-Jona-Lasino Model with Semi-Classical Approximation

Impossibility of Spin Polarized States for Neutron Star / Proto-neutron Star Matter in β-Equilibrium Condition

Impossibility of Spin Polarized States for Neutron Star / Proto-neutron Star Matter in $β$ -Equilibrium Condition