Relativistic version of Landau theory of Fermi liquid in presence of strong quantizing magnetic field—an exact formalism

Ghosh, Sutapa; Mandal, Satyendra Nath; Chakrabarty, Somenath

doi:10.1016/j.aop.2004.03.001

Cited by 7 publications

(10 citation statements)

References 22 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…( 18). This agrees with the corresponding relativistic Fermi liquid (and zero magnetic field) formula of [23] and with the result of [25]. We should also mention that the zero sound velocity v 0 should be obviously smaller than the speed of light.…”

Section: Zero Sound Modessupporting

confidence: 90%

Zero sound in neutron stars with dense quark matter under strong magnetic fields

Kouvaris¹

2009

Phys. Rev. D

View full text Add to dashboard Cite

We study a neutron star with a quark matter core under extremely strong magnetic fields. We investigate the possibility of an Urca process as a mechanism for the cooling of such a star. We found that apart from very particular cases, the Urca process cannot occur. We also study the stability of zero sound modes under the same conditions. We derive limits for the coupling constant of an effective theory, in order the zero sound to be undamped. We show that zero sound modes can help kinematically to facilitate a cooling process. * Electronic address: kouvaris@nbi.dk

show abstract

Section: Zero Sound Modessupporting

confidence: 90%

Zero sound in neutron stars with dense quark matter under strong magnetic fields

Kouvaris¹

2009

Phys. Rev. D

View full text Add to dashboard Cite

show abstract

“…Now similar to the conventional nonrelativistic model of Landau theory of Fermi liquid, this modified version also deals with normal Fermi liquid and is applicable for the low-lying excited states of the system, which consists of a superposition of quasi-particle excitation close to the Fermi surface. The formalism we have developed in this article is basically a re-formulation of our previous work [29] and an extension of a very old paper by Baym and Chin [30]. Of course, in the present investigation, we have found a new and interesting result, the complex nature of nucleonic self energies in the mean field approximation.…”

Section: Introductionmentioning

confidence: 54%

“…2 ) These set of relations are also totally new results and have been derived in our previous publication [29]. Then we have following Baym and Chin [30] …”

Section: Scalar Boson Exchangementioning

confidence: 74%

“…In one of our recent studies, we have developed a relativistic formalism of Landau theory of Fermi liquid for dense neutron star matter in presence of strong quantizing magnetic field with σ − ω meson exchange [29]. In the present article we shall re-formulate our previous work as cited above, incorporating ρ-meson (both charged and neutral components) exchange interactions.…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Neutron star equation of state and the possibility of complex self-energy in Landau theory of a Fermi liquid in the presence of a strong, quantizing magnetic field

et al. 2006

Self Cite

View full text Add to dashboard Cite

Using the relativistic version of Landau theory of Fermi liquid with σ − ω and ρ mesons exchange, we have obtained an equation state for dense neutron star matter in presence of strong quantizing magnetic field. It is found that in this scenario the self-energies of both neutron and proton components of dense neutron star matter become complex under certain physical conditions. To be more specific, it is observed that in the exchange diagrams of σ, ω and neutral ρ transfer processes and in the direct interaction diagram with ρ± transfer reactions, the nucleon self-energies become complex in nature.

show abstract

“…We shall follow some of our recent studies where we have developed a relativistic formalism of Landau theory of Fermi liquid for dense neutron star matter in presence of strong quantizing magnetic field with the exchange of σ -ω-ρ mesons (Ghosh et al 2004;Mandal et al 2006). We have noticed that the densities of both proton and neutron components, which are in β-equilibrium are functions of magnetic field strength.…”

mentioning

confidence: 97%

The upper limit of magnetic field strength in dense stellar hadronic matter

Chakrabarty

2007

Astrophys Space Sci

Self Cite

View full text Add to dashboard Cite

It is shown that in strongly magnetized neutron stars, there exist upper limits of magnetic field strength, beyond which the self energies for both neutron and proton components of neutron star matter become complex in nature. As a consequence they decay within the strong interaction time scale. However, in the ultra-strong magnetic field case, when the zeroth Landau level is only occupied by protons, the system again becomes stable against strong decay.Keywords Magnetar · Magnetic field · Neutron stars · Landau levels PACS 97.60.Jd · 97.60.-s · 75.25.+zThe study of the effect of strong quantizing magnetic fields on dense neutron star matter has become extremely interesting and also important after the recent discovery of a few strongly magnetized neutron stars, known as magnetars (Duncan and These strange stellar objects are supposed to be relatively young (age ∼10 4 yrs) neutron stars and are also believed to be the possible sources of anomalous X-ray pulses and soft gamma ray emissions (AXP and SGR). If the magnetic fields are strong enough, particularly at the central region, then most of the physical properties of these strange stellar objects and also various physical processes taking place

show abstract

Relativistic version of Landau theory of Fermi liquid in presence of strong quantizing magnetic field—an exact formalism

Abstract: PACS :97.60.Jd, 75.25.+z An exact formalism for the relativistic version of Landau theory of Fermi liquid in presence of strong quantizing magnetic field is developed. Both direct and exchange type interactions with scalar and vector coupling cases are considered.

Cited by 7 publications

References 22 publications

Zero sound in neutron stars with dense quark matter under strong magnetic fields

Zero sound in neutron stars with dense quark matter under strong magnetic fields

Neutron star equation of state and the possibility of complex self-energy in Landau theory of a Fermi liquid in the presence of a strong, quantizing magnetic field

The upper limit of magnetic field strength in dense stellar hadronic matter

Contact Info

Product

Resources

About