Acoustic modal instability in relativistic gyromagnetoactive ultra-dense quantum fluids
Abstract The acoustic modal instability excitable in a relativistic gyromagnetoactive quantum plasma model is methodologically investigated. The proposed spherical model consists of fully degenerate relativistic electronic species, governed by an appropriate barotropic equation of state sourced in t...
Ausführliche Beschreibung
Gespeichert in:
| Autor*in: |
Dasgupta, Sayanti [verfasserIn] |
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| Format: |
E-Artikel |
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| Sprache: |
Englisch |
| Erschienen: |
2022 |
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| Schlagwörter: |
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| Anmerkung: |
© Indian Academy of Sciences 2022 |
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| Übergeordnetes Werk: |
Enthalten in: Journal of astrophysics and astronomy - Bangalore : Springer India, 1980, 43(2022), 2 vom: 03. Sept. |
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| Übergeordnetes Werk: |
volume:43 ; year:2022 ; number:2 ; day:03 ; month:09 |
| Links: |
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| DOI / URN: |
10.1007/s12036-022-09836-5 |
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| Katalog-ID: |
SPR048016047 |
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| 100 | 1 | |a Dasgupta, Sayanti |e verfasserin |4 aut | |
| 245 | 1 | 0 | |a Acoustic modal instability in relativistic gyromagnetoactive ultra-dense quantum fluids |
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| 520 | |a Abstract The acoustic modal instability excitable in a relativistic gyromagnetoactive quantum plasma model is methodologically investigated. The proposed spherical model consists of fully degenerate relativistic electronic species, governed by an appropriate barotropic equation of state sourced in the gyrokinetic water-bag distribution. The tiny degenerate electronic species is responsible for providing the outward elastic force. The heavier relativistic singly charged ionic species provides the required inertial force for sustaining the acoustic instability mode excitation under consideration. It includes the co-action of the quantum diffraction effects, Coriolis rotation, electrostatic confinement pressure, Lorentz force fields, etc. A standard normal spherical mode analysis yields a generalized quartic linear dispersion relation dictated by a unique set of multiparametric coefficients. A numerical illustrative platform is provided to analyze the instability behaviours in two extreme regimes (ULF plus UHF). A good number of new and interesting stability properties in response to parametric variations are derived, discussed and established. It could be useful to see the acoustic wave stability features naturalistically excitable in the compact astrophysical class of bounded structures, such as brown dwarfs, white dwarfs and neutron stars. | ||
| 650 | 4 | |a Acoustic mode |7 (dpeaa)DE-He213 | |
| 650 | 4 | |a relativistic quantum plasmas |7 (dpeaa)DE-He213 | |
| 650 | 4 | |a dwarf stars |7 (dpeaa)DE-He213 | |
| 700 | 1 | |a Karmakar, Pralay Kumar |0 (orcid)0000-0003-0898-4166 |4 aut | |
| 773 | 0 | 8 | |i Enthalten in |t Journal of astrophysics and astronomy |d Bangalore : Springer India, 1980 |g 43(2022), 2 vom: 03. Sept. |w (DE-627)358454131 |w (DE-600)2096381-6 |x 0973-7758 |7 nnns |
| 773 | 1 | 8 | |g volume:43 |g year:2022 |g number:2 |g day:03 |g month:09 |
| 856 | 4 | 0 | |u https://dx.doi.org/10.1007/s12036-022-09836-5 |z lizenzpflichtig |3 Volltext |
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10.1007/s12036-022-09836-5 doi (DE-627)SPR048016047 (SPR)s12036-022-09836-5-e DE-627 ger DE-627 rakwb eng Dasgupta, Sayanti verfasserin aut Acoustic modal instability in relativistic gyromagnetoactive ultra-dense quantum fluids 2022 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier © Indian Academy of Sciences 2022 Abstract The acoustic modal instability excitable in a relativistic gyromagnetoactive quantum plasma model is methodologically investigated. The proposed spherical model consists of fully degenerate relativistic electronic species, governed by an appropriate barotropic equation of state sourced in the gyrokinetic water-bag distribution. The tiny degenerate electronic species is responsible for providing the outward elastic force. The heavier relativistic singly charged ionic species provides the required inertial force for sustaining the acoustic instability mode excitation under consideration. It includes the co-action of the quantum diffraction effects, Coriolis rotation, electrostatic confinement pressure, Lorentz force fields, etc. A standard normal spherical mode analysis yields a generalized quartic linear dispersion relation dictated by a unique set of multiparametric coefficients. A numerical illustrative platform is provided to analyze the instability behaviours in two extreme regimes (ULF plus UHF). A good number of new and interesting stability properties in response to parametric variations are derived, discussed and established. It could be useful to see the acoustic wave stability features naturalistically excitable in the compact astrophysical class of bounded structures, such as brown dwarfs, white dwarfs and neutron stars. Acoustic mode (dpeaa)DE-He213 relativistic quantum plasmas (dpeaa)DE-He213 dwarf stars (dpeaa)DE-He213 Karmakar, Pralay Kumar (orcid)0000-0003-0898-4166 aut Enthalten in Journal of astrophysics and astronomy Bangalore : Springer India, 1980 43(2022), 2 vom: 03. Sept. (DE-627)358454131 (DE-600)2096381-6 0973-7758 nnns volume:43 year:2022 number:2 day:03 month:09 https://dx.doi.org/10.1007/s12036-022-09836-5 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_138 GBV_ILN_150 GBV_ILN_151 GBV_ILN_152 GBV_ILN_161 GBV_ILN_170 GBV_ILN_171 GBV_ILN_187 GBV_ILN_206 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_636 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2056 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2088 GBV_ILN_2093 GBV_ILN_2106 GBV_ILN_2107 GBV_ILN_2108 GBV_ILN_2110 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2118 GBV_ILN_2119 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2188 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_2336 GBV_ILN_2446 GBV_ILN_2470 GBV_ILN_2472 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_2548 GBV_ILN_4012 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4242 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4251 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4326 GBV_ILN_4328 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4336 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4393 GBV_ILN_4700 AR 43 2022 2 03 09 |
| spelling |
10.1007/s12036-022-09836-5 doi (DE-627)SPR048016047 (SPR)s12036-022-09836-5-e DE-627 ger DE-627 rakwb eng Dasgupta, Sayanti verfasserin aut Acoustic modal instability in relativistic gyromagnetoactive ultra-dense quantum fluids 2022 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier © Indian Academy of Sciences 2022 Abstract The acoustic modal instability excitable in a relativistic gyromagnetoactive quantum plasma model is methodologically investigated. The proposed spherical model consists of fully degenerate relativistic electronic species, governed by an appropriate barotropic equation of state sourced in the gyrokinetic water-bag distribution. The tiny degenerate electronic species is responsible for providing the outward elastic force. The heavier relativistic singly charged ionic species provides the required inertial force for sustaining the acoustic instability mode excitation under consideration. It includes the co-action of the quantum diffraction effects, Coriolis rotation, electrostatic confinement pressure, Lorentz force fields, etc. A standard normal spherical mode analysis yields a generalized quartic linear dispersion relation dictated by a unique set of multiparametric coefficients. A numerical illustrative platform is provided to analyze the instability behaviours in two extreme regimes (ULF plus UHF). A good number of new and interesting stability properties in response to parametric variations are derived, discussed and established. It could be useful to see the acoustic wave stability features naturalistically excitable in the compact astrophysical class of bounded structures, such as brown dwarfs, white dwarfs and neutron stars. Acoustic mode (dpeaa)DE-He213 relativistic quantum plasmas (dpeaa)DE-He213 dwarf stars (dpeaa)DE-He213 Karmakar, Pralay Kumar (orcid)0000-0003-0898-4166 aut Enthalten in Journal of astrophysics and astronomy Bangalore : Springer India, 1980 43(2022), 2 vom: 03. Sept. (DE-627)358454131 (DE-600)2096381-6 0973-7758 nnns volume:43 year:2022 number:2 day:03 month:09 https://dx.doi.org/10.1007/s12036-022-09836-5 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_138 GBV_ILN_150 GBV_ILN_151 GBV_ILN_152 GBV_ILN_161 GBV_ILN_170 GBV_ILN_171 GBV_ILN_187 GBV_ILN_206 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_636 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2056 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2088 GBV_ILN_2093 GBV_ILN_2106 GBV_ILN_2107 GBV_ILN_2108 GBV_ILN_2110 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2118 GBV_ILN_2119 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2188 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_2336 GBV_ILN_2446 GBV_ILN_2470 GBV_ILN_2472 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_2548 GBV_ILN_4012 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4242 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4251 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4326 GBV_ILN_4328 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4336 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4393 GBV_ILN_4700 AR 43 2022 2 03 09 |
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10.1007/s12036-022-09836-5 doi (DE-627)SPR048016047 (SPR)s12036-022-09836-5-e DE-627 ger DE-627 rakwb eng Dasgupta, Sayanti verfasserin aut Acoustic modal instability in relativistic gyromagnetoactive ultra-dense quantum fluids 2022 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier © Indian Academy of Sciences 2022 Abstract The acoustic modal instability excitable in a relativistic gyromagnetoactive quantum plasma model is methodologically investigated. The proposed spherical model consists of fully degenerate relativistic electronic species, governed by an appropriate barotropic equation of state sourced in the gyrokinetic water-bag distribution. The tiny degenerate electronic species is responsible for providing the outward elastic force. The heavier relativistic singly charged ionic species provides the required inertial force for sustaining the acoustic instability mode excitation under consideration. It includes the co-action of the quantum diffraction effects, Coriolis rotation, electrostatic confinement pressure, Lorentz force fields, etc. A standard normal spherical mode analysis yields a generalized quartic linear dispersion relation dictated by a unique set of multiparametric coefficients. A numerical illustrative platform is provided to analyze the instability behaviours in two extreme regimes (ULF plus UHF). A good number of new and interesting stability properties in response to parametric variations are derived, discussed and established. It could be useful to see the acoustic wave stability features naturalistically excitable in the compact astrophysical class of bounded structures, such as brown dwarfs, white dwarfs and neutron stars. Acoustic mode (dpeaa)DE-He213 relativistic quantum plasmas (dpeaa)DE-He213 dwarf stars (dpeaa)DE-He213 Karmakar, Pralay Kumar (orcid)0000-0003-0898-4166 aut Enthalten in Journal of astrophysics and astronomy Bangalore : Springer India, 1980 43(2022), 2 vom: 03. Sept. (DE-627)358454131 (DE-600)2096381-6 0973-7758 nnns volume:43 year:2022 number:2 day:03 month:09 https://dx.doi.org/10.1007/s12036-022-09836-5 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_138 GBV_ILN_150 GBV_ILN_151 GBV_ILN_152 GBV_ILN_161 GBV_ILN_170 GBV_ILN_171 GBV_ILN_187 GBV_ILN_206 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_636 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2056 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2088 GBV_ILN_2093 GBV_ILN_2106 GBV_ILN_2107 GBV_ILN_2108 GBV_ILN_2110 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2118 GBV_ILN_2119 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2188 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_2336 GBV_ILN_2446 GBV_ILN_2470 GBV_ILN_2472 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_2548 GBV_ILN_4012 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4242 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4251 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4326 GBV_ILN_4328 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4336 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4393 GBV_ILN_4700 AR 43 2022 2 03 09 |
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10.1007/s12036-022-09836-5 doi (DE-627)SPR048016047 (SPR)s12036-022-09836-5-e DE-627 ger DE-627 rakwb eng Dasgupta, Sayanti verfasserin aut Acoustic modal instability in relativistic gyromagnetoactive ultra-dense quantum fluids 2022 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier © Indian Academy of Sciences 2022 Abstract The acoustic modal instability excitable in a relativistic gyromagnetoactive quantum plasma model is methodologically investigated. The proposed spherical model consists of fully degenerate relativistic electronic species, governed by an appropriate barotropic equation of state sourced in the gyrokinetic water-bag distribution. The tiny degenerate electronic species is responsible for providing the outward elastic force. The heavier relativistic singly charged ionic species provides the required inertial force for sustaining the acoustic instability mode excitation under consideration. It includes the co-action of the quantum diffraction effects, Coriolis rotation, electrostatic confinement pressure, Lorentz force fields, etc. A standard normal spherical mode analysis yields a generalized quartic linear dispersion relation dictated by a unique set of multiparametric coefficients. A numerical illustrative platform is provided to analyze the instability behaviours in two extreme regimes (ULF plus UHF). A good number of new and interesting stability properties in response to parametric variations are derived, discussed and established. It could be useful to see the acoustic wave stability features naturalistically excitable in the compact astrophysical class of bounded structures, such as brown dwarfs, white dwarfs and neutron stars. Acoustic mode (dpeaa)DE-He213 relativistic quantum plasmas (dpeaa)DE-He213 dwarf stars (dpeaa)DE-He213 Karmakar, Pralay Kumar (orcid)0000-0003-0898-4166 aut Enthalten in Journal of astrophysics and astronomy Bangalore : Springer India, 1980 43(2022), 2 vom: 03. Sept. (DE-627)358454131 (DE-600)2096381-6 0973-7758 nnns volume:43 year:2022 number:2 day:03 month:09 https://dx.doi.org/10.1007/s12036-022-09836-5 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_138 GBV_ILN_150 GBV_ILN_151 GBV_ILN_152 GBV_ILN_161 GBV_ILN_170 GBV_ILN_171 GBV_ILN_187 GBV_ILN_206 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_636 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2056 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2088 GBV_ILN_2093 GBV_ILN_2106 GBV_ILN_2107 GBV_ILN_2108 GBV_ILN_2110 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2118 GBV_ILN_2119 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2188 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_2336 GBV_ILN_2446 GBV_ILN_2470 GBV_ILN_2472 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_2548 GBV_ILN_4012 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4242 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4251 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4326 GBV_ILN_4328 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4336 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4393 GBV_ILN_4700 AR 43 2022 2 03 09 |
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10.1007/s12036-022-09836-5 doi (DE-627)SPR048016047 (SPR)s12036-022-09836-5-e DE-627 ger DE-627 rakwb eng Dasgupta, Sayanti verfasserin aut Acoustic modal instability in relativistic gyromagnetoactive ultra-dense quantum fluids 2022 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier © Indian Academy of Sciences 2022 Abstract The acoustic modal instability excitable in a relativistic gyromagnetoactive quantum plasma model is methodologically investigated. The proposed spherical model consists of fully degenerate relativistic electronic species, governed by an appropriate barotropic equation of state sourced in the gyrokinetic water-bag distribution. The tiny degenerate electronic species is responsible for providing the outward elastic force. The heavier relativistic singly charged ionic species provides the required inertial force for sustaining the acoustic instability mode excitation under consideration. It includes the co-action of the quantum diffraction effects, Coriolis rotation, electrostatic confinement pressure, Lorentz force fields, etc. A standard normal spherical mode analysis yields a generalized quartic linear dispersion relation dictated by a unique set of multiparametric coefficients. A numerical illustrative platform is provided to analyze the instability behaviours in two extreme regimes (ULF plus UHF). A good number of new and interesting stability properties in response to parametric variations are derived, discussed and established. It could be useful to see the acoustic wave stability features naturalistically excitable in the compact astrophysical class of bounded structures, such as brown dwarfs, white dwarfs and neutron stars. Acoustic mode (dpeaa)DE-He213 relativistic quantum plasmas (dpeaa)DE-He213 dwarf stars (dpeaa)DE-He213 Karmakar, Pralay Kumar (orcid)0000-0003-0898-4166 aut Enthalten in Journal of astrophysics and astronomy Bangalore : Springer India, 1980 43(2022), 2 vom: 03. Sept. (DE-627)358454131 (DE-600)2096381-6 0973-7758 nnns volume:43 year:2022 number:2 day:03 month:09 https://dx.doi.org/10.1007/s12036-022-09836-5 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_138 GBV_ILN_150 GBV_ILN_151 GBV_ILN_152 GBV_ILN_161 GBV_ILN_170 GBV_ILN_171 GBV_ILN_187 GBV_ILN_206 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_636 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2056 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2088 GBV_ILN_2093 GBV_ILN_2106 GBV_ILN_2107 GBV_ILN_2108 GBV_ILN_2110 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2118 GBV_ILN_2119 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2188 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_2336 GBV_ILN_2446 GBV_ILN_2470 GBV_ILN_2472 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_2548 GBV_ILN_4012 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4242 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4251 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4326 GBV_ILN_4328 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4336 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4393 GBV_ILN_4700 AR 43 2022 2 03 09 |
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Dasgupta, Sayanti |
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Dasgupta, Sayanti misc Acoustic mode misc relativistic quantum plasmas misc dwarf stars Acoustic modal instability in relativistic gyromagnetoactive ultra-dense quantum fluids |
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Acoustic modal instability in relativistic gyromagnetoactive ultra-dense quantum fluids Acoustic mode (dpeaa)DE-He213 relativistic quantum plasmas (dpeaa)DE-He213 dwarf stars (dpeaa)DE-He213 |
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Acoustic modal instability in relativistic gyromagnetoactive ultra-dense quantum fluids |
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acoustic modal instability in relativistic gyromagnetoactive ultra-dense quantum fluids |
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Acoustic modal instability in relativistic gyromagnetoactive ultra-dense quantum fluids |
| abstract |
Abstract The acoustic modal instability excitable in a relativistic gyromagnetoactive quantum plasma model is methodologically investigated. The proposed spherical model consists of fully degenerate relativistic electronic species, governed by an appropriate barotropic equation of state sourced in the gyrokinetic water-bag distribution. The tiny degenerate electronic species is responsible for providing the outward elastic force. The heavier relativistic singly charged ionic species provides the required inertial force for sustaining the acoustic instability mode excitation under consideration. It includes the co-action of the quantum diffraction effects, Coriolis rotation, electrostatic confinement pressure, Lorentz force fields, etc. A standard normal spherical mode analysis yields a generalized quartic linear dispersion relation dictated by a unique set of multiparametric coefficients. A numerical illustrative platform is provided to analyze the instability behaviours in two extreme regimes (ULF plus UHF). A good number of new and interesting stability properties in response to parametric variations are derived, discussed and established. It could be useful to see the acoustic wave stability features naturalistically excitable in the compact astrophysical class of bounded structures, such as brown dwarfs, white dwarfs and neutron stars. © Indian Academy of Sciences 2022 |
| abstractGer |
Abstract The acoustic modal instability excitable in a relativistic gyromagnetoactive quantum plasma model is methodologically investigated. The proposed spherical model consists of fully degenerate relativistic electronic species, governed by an appropriate barotropic equation of state sourced in the gyrokinetic water-bag distribution. The tiny degenerate electronic species is responsible for providing the outward elastic force. The heavier relativistic singly charged ionic species provides the required inertial force for sustaining the acoustic instability mode excitation under consideration. It includes the co-action of the quantum diffraction effects, Coriolis rotation, electrostatic confinement pressure, Lorentz force fields, etc. A standard normal spherical mode analysis yields a generalized quartic linear dispersion relation dictated by a unique set of multiparametric coefficients. A numerical illustrative platform is provided to analyze the instability behaviours in two extreme regimes (ULF plus UHF). A good number of new and interesting stability properties in response to parametric variations are derived, discussed and established. It could be useful to see the acoustic wave stability features naturalistically excitable in the compact astrophysical class of bounded structures, such as brown dwarfs, white dwarfs and neutron stars. © Indian Academy of Sciences 2022 |
| abstract_unstemmed |
Abstract The acoustic modal instability excitable in a relativistic gyromagnetoactive quantum plasma model is methodologically investigated. The proposed spherical model consists of fully degenerate relativistic electronic species, governed by an appropriate barotropic equation of state sourced in the gyrokinetic water-bag distribution. The tiny degenerate electronic species is responsible for providing the outward elastic force. The heavier relativistic singly charged ionic species provides the required inertial force for sustaining the acoustic instability mode excitation under consideration. It includes the co-action of the quantum diffraction effects, Coriolis rotation, electrostatic confinement pressure, Lorentz force fields, etc. A standard normal spherical mode analysis yields a generalized quartic linear dispersion relation dictated by a unique set of multiparametric coefficients. A numerical illustrative platform is provided to analyze the instability behaviours in two extreme regimes (ULF plus UHF). A good number of new and interesting stability properties in response to parametric variations are derived, discussed and established. It could be useful to see the acoustic wave stability features naturalistically excitable in the compact astrophysical class of bounded structures, such as brown dwarfs, white dwarfs and neutron stars. © Indian Academy of Sciences 2022 |
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Acoustic modal instability in relativistic gyromagnetoactive ultra-dense quantum fluids |
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https://dx.doi.org/10.1007/s12036-022-09836-5 |
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Karmakar, Pralay Kumar |
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| doi_str |
10.1007/s12036-022-09836-5 |
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2024-07-03T16:27:35.623Z |
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