Mass Evolution of Schwarzschild Black Holes

Abstract In the classical theory of general relativity, black holes can only absorb and not emit particles. When quantum mechanical effects are taken into account, then the black holes emit particles as hot bodies with temperature proportional to κ, its surface gravity. This thermal emission can lea...
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Gespeichert in:

Autor*in:	de Santi, Natalí Soler Matubaro [verfasserIn] Santarelli, Raphael [verfasserIn]

Format:	E-Artikel
Sprache:	Englisch

Erschienen:	2019

Schlagwörter:	Black hole thermodynamics Black hole evaporation Mass evolution of black holes Schwarzschild black hole

Übergeordnetes Werk:	Enthalten in: Brazilian journal of physics - New York, NY : Springer New York, 1996, 49(2019), 6 vom: 31. Okt., Seite 897-913
Übergeordnetes Werk:	volume:49 ; year:2019 ; number:6 ; day:31 ; month:10 ; pages:897-913

Links:	Volltext

DOI / URN:	10.1007/s13538-019-00708-y

Katalog-ID:	SPR031751326

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520			\|a Abstract In the classical theory of general relativity, black holes can only absorb and not emit particles. When quantum mechanical effects are taken into account, then the black holes emit particles as hot bodies with temperature proportional to κ, its surface gravity. This thermal emission can lead to a slow decrease in the mass of the black hole, and eventually to its disappearance, also called black hole evaporation. This characteristic allows us to analyze what happens with the mass of the black hole when its temperature is increased or decreased and how the energy is exchanged with the external environment. This paper has the aim to make a discussion about the mass evolution, due to Hawking radiation emission, of Schwarzschild black holes with different initial masses and external conditions as the empty space, the cosmic microwave background with constant temperature, and with temperature varying in accordance with the eras of the universe. Our main contributions are to take into account these variations in the temperature of the cosmic background radiation and use them into the black holes dynamics and also to analyze the asymptotic behavior of the solutions. As a result, we have the complete evaporation of the black holes in most cases, although their masses can increase in some cases, and even diverge for specific conditions.
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matchkey_str	article:16784448:2019----::asvltooshazci
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bklnumber	33.00
publishDate	2019
allfields	10.1007/s13538-019-00708-y doi (DE-627)SPR031751326 (SPR)s13538-019-00708-y-e DE-627 ger DE-627 rakwb eng 530 ASE 33.00 bkl de Santi, Natalí Soler Matubaro verfasserin aut Mass Evolution of Schwarzschild Black Holes 2019 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract In the classical theory of general relativity, black holes can only absorb and not emit particles. When quantum mechanical effects are taken into account, then the black holes emit particles as hot bodies with temperature proportional to κ, its surface gravity. This thermal emission can lead to a slow decrease in the mass of the black hole, and eventually to its disappearance, also called black hole evaporation. This characteristic allows us to analyze what happens with the mass of the black hole when its temperature is increased or decreased and how the energy is exchanged with the external environment. This paper has the aim to make a discussion about the mass evolution, due to Hawking radiation emission, of Schwarzschild black holes with different initial masses and external conditions as the empty space, the cosmic microwave background with constant temperature, and with temperature varying in accordance with the eras of the universe. Our main contributions are to take into account these variations in the temperature of the cosmic background radiation and use them into the black holes dynamics and also to analyze the asymptotic behavior of the solutions. As a result, we have the complete evaporation of the black holes in most cases, although their masses can increase in some cases, and even diverge for specific conditions. Black hole thermodynamics (dpeaa)DE-He213 Black hole evaporation (dpeaa)DE-He213 Mass evolution of black holes (dpeaa)DE-He213 Schwarzschild black hole (dpeaa)DE-He213 Santarelli, Raphael verfasserin aut Enthalten in Brazilian journal of physics New York, NY : Springer New York, 1996 49(2019), 6 vom: 31. Okt., Seite 897-913 (DE-627)302928243 (DE-600)1493260-X 1678-4448 nnns volume:49 year:2019 number:6 day:31 month:10 pages:897-913 https://dx.doi.org/10.1007/s13538-019-00708-y 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_101 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_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_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2070 GBV_ILN_2086 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_2116 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_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 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_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4336 GBV_ILN_4338 GBV_ILN_4393 GBV_ILN_4700 33.00 ASE AR 49 2019 6 31 10 897-913
spelling	10.1007/s13538-019-00708-y doi (DE-627)SPR031751326 (SPR)s13538-019-00708-y-e DE-627 ger DE-627 rakwb eng 530 ASE 33.00 bkl de Santi, Natalí Soler Matubaro verfasserin aut Mass Evolution of Schwarzschild Black Holes 2019 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract In the classical theory of general relativity, black holes can only absorb and not emit particles. When quantum mechanical effects are taken into account, then the black holes emit particles as hot bodies with temperature proportional to κ, its surface gravity. This thermal emission can lead to a slow decrease in the mass of the black hole, and eventually to its disappearance, also called black hole evaporation. This characteristic allows us to analyze what happens with the mass of the black hole when its temperature is increased or decreased and how the energy is exchanged with the external environment. This paper has the aim to make a discussion about the mass evolution, due to Hawking radiation emission, of Schwarzschild black holes with different initial masses and external conditions as the empty space, the cosmic microwave background with constant temperature, and with temperature varying in accordance with the eras of the universe. Our main contributions are to take into account these variations in the temperature of the cosmic background radiation and use them into the black holes dynamics and also to analyze the asymptotic behavior of the solutions. As a result, we have the complete evaporation of the black holes in most cases, although their masses can increase in some cases, and even diverge for specific conditions. Black hole thermodynamics (dpeaa)DE-He213 Black hole evaporation (dpeaa)DE-He213 Mass evolution of black holes (dpeaa)DE-He213 Schwarzschild black hole (dpeaa)DE-He213 Santarelli, Raphael verfasserin aut Enthalten in Brazilian journal of physics New York, NY : Springer New York, 1996 49(2019), 6 vom: 31. Okt., Seite 897-913 (DE-627)302928243 (DE-600)1493260-X 1678-4448 nnns volume:49 year:2019 number:6 day:31 month:10 pages:897-913 https://dx.doi.org/10.1007/s13538-019-00708-y 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_101 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_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_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2070 GBV_ILN_2086 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_2116 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_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 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_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4336 GBV_ILN_4338 GBV_ILN_4393 GBV_ILN_4700 33.00 ASE AR 49 2019 6 31 10 897-913
allfields_unstemmed	10.1007/s13538-019-00708-y doi (DE-627)SPR031751326 (SPR)s13538-019-00708-y-e DE-627 ger DE-627 rakwb eng 530 ASE 33.00 bkl de Santi, Natalí Soler Matubaro verfasserin aut Mass Evolution of Schwarzschild Black Holes 2019 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract In the classical theory of general relativity, black holes can only absorb and not emit particles. When quantum mechanical effects are taken into account, then the black holes emit particles as hot bodies with temperature proportional to κ, its surface gravity. This thermal emission can lead to a slow decrease in the mass of the black hole, and eventually to its disappearance, also called black hole evaporation. This characteristic allows us to analyze what happens with the mass of the black hole when its temperature is increased or decreased and how the energy is exchanged with the external environment. This paper has the aim to make a discussion about the mass evolution, due to Hawking radiation emission, of Schwarzschild black holes with different initial masses and external conditions as the empty space, the cosmic microwave background with constant temperature, and with temperature varying in accordance with the eras of the universe. Our main contributions are to take into account these variations in the temperature of the cosmic background radiation and use them into the black holes dynamics and also to analyze the asymptotic behavior of the solutions. As a result, we have the complete evaporation of the black holes in most cases, although their masses can increase in some cases, and even diverge for specific conditions. Black hole thermodynamics (dpeaa)DE-He213 Black hole evaporation (dpeaa)DE-He213 Mass evolution of black holes (dpeaa)DE-He213 Schwarzschild black hole (dpeaa)DE-He213 Santarelli, Raphael verfasserin aut Enthalten in Brazilian journal of physics New York, NY : Springer New York, 1996 49(2019), 6 vom: 31. Okt., Seite 897-913 (DE-627)302928243 (DE-600)1493260-X 1678-4448 nnns volume:49 year:2019 number:6 day:31 month:10 pages:897-913 https://dx.doi.org/10.1007/s13538-019-00708-y 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_101 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_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_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2070 GBV_ILN_2086 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_2116 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_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 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_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4336 GBV_ILN_4338 GBV_ILN_4393 GBV_ILN_4700 33.00 ASE AR 49 2019 6 31 10 897-913
allfieldsGer	10.1007/s13538-019-00708-y doi (DE-627)SPR031751326 (SPR)s13538-019-00708-y-e DE-627 ger DE-627 rakwb eng 530 ASE 33.00 bkl de Santi, Natalí Soler Matubaro verfasserin aut Mass Evolution of Schwarzschild Black Holes 2019 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract In the classical theory of general relativity, black holes can only absorb and not emit particles. When quantum mechanical effects are taken into account, then the black holes emit particles as hot bodies with temperature proportional to κ, its surface gravity. This thermal emission can lead to a slow decrease in the mass of the black hole, and eventually to its disappearance, also called black hole evaporation. This characteristic allows us to analyze what happens with the mass of the black hole when its temperature is increased or decreased and how the energy is exchanged with the external environment. This paper has the aim to make a discussion about the mass evolution, due to Hawking radiation emission, of Schwarzschild black holes with different initial masses and external conditions as the empty space, the cosmic microwave background with constant temperature, and with temperature varying in accordance with the eras of the universe. Our main contributions are to take into account these variations in the temperature of the cosmic background radiation and use them into the black holes dynamics and also to analyze the asymptotic behavior of the solutions. As a result, we have the complete evaporation of the black holes in most cases, although their masses can increase in some cases, and even diverge for specific conditions. Black hole thermodynamics (dpeaa)DE-He213 Black hole evaporation (dpeaa)DE-He213 Mass evolution of black holes (dpeaa)DE-He213 Schwarzschild black hole (dpeaa)DE-He213 Santarelli, Raphael verfasserin aut Enthalten in Brazilian journal of physics New York, NY : Springer New York, 1996 49(2019), 6 vom: 31. Okt., Seite 897-913 (DE-627)302928243 (DE-600)1493260-X 1678-4448 nnns volume:49 year:2019 number:6 day:31 month:10 pages:897-913 https://dx.doi.org/10.1007/s13538-019-00708-y 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_101 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_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_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2070 GBV_ILN_2086 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_2116 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_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 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_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4336 GBV_ILN_4338 GBV_ILN_4393 GBV_ILN_4700 33.00 ASE AR 49 2019 6 31 10 897-913
allfieldsSound	10.1007/s13538-019-00708-y doi (DE-627)SPR031751326 (SPR)s13538-019-00708-y-e DE-627 ger DE-627 rakwb eng 530 ASE 33.00 bkl de Santi, Natalí Soler Matubaro verfasserin aut Mass Evolution of Schwarzschild Black Holes 2019 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract In the classical theory of general relativity, black holes can only absorb and not emit particles. When quantum mechanical effects are taken into account, then the black holes emit particles as hot bodies with temperature proportional to κ, its surface gravity. This thermal emission can lead to a slow decrease in the mass of the black hole, and eventually to its disappearance, also called black hole evaporation. This characteristic allows us to analyze what happens with the mass of the black hole when its temperature is increased or decreased and how the energy is exchanged with the external environment. This paper has the aim to make a discussion about the mass evolution, due to Hawking radiation emission, of Schwarzschild black holes with different initial masses and external conditions as the empty space, the cosmic microwave background with constant temperature, and with temperature varying in accordance with the eras of the universe. Our main contributions are to take into account these variations in the temperature of the cosmic background radiation and use them into the black holes dynamics and also to analyze the asymptotic behavior of the solutions. As a result, we have the complete evaporation of the black holes in most cases, although their masses can increase in some cases, and even diverge for specific conditions. Black hole thermodynamics (dpeaa)DE-He213 Black hole evaporation (dpeaa)DE-He213 Mass evolution of black holes (dpeaa)DE-He213 Schwarzschild black hole (dpeaa)DE-He213 Santarelli, Raphael verfasserin aut Enthalten in Brazilian journal of physics New York, NY : Springer New York, 1996 49(2019), 6 vom: 31. Okt., Seite 897-913 (DE-627)302928243 (DE-600)1493260-X 1678-4448 nnns volume:49 year:2019 number:6 day:31 month:10 pages:897-913 https://dx.doi.org/10.1007/s13538-019-00708-y 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_101 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_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_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2070 GBV_ILN_2086 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_2116 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_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 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_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4336 GBV_ILN_4338 GBV_ILN_4393 GBV_ILN_4700 33.00 ASE AR 49 2019 6 31 10 897-913
language	English
source	Enthalten in Brazilian journal of physics 49(2019), 6 vom: 31. Okt., Seite 897-913 volume:49 year:2019 number:6 day:31 month:10 pages:897-913
sourceStr	Enthalten in Brazilian journal of physics 49(2019), 6 vom: 31. Okt., Seite 897-913 volume:49 year:2019 number:6 day:31 month:10 pages:897-913
format_phy_str_mv	Article
institution	findex.gbv.de
topic_facet	Black hole thermodynamics Black hole evaporation Mass evolution of black holes Schwarzschild black hole
dewey-raw	530
isfreeaccess_bool	false
container_title	Brazilian journal of physics
authorswithroles_txt_mv	de Santi, Natalí Soler Matubaro @@aut@@ Santarelli, Raphael @@aut@@
publishDateDaySort_date	2019-10-31T00:00:00Z
hierarchy_top_id	302928243
dewey-sort	3530
id	SPR031751326
language_de	englisch
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author	de Santi, Natalí Soler Matubaro
spellingShingle	de Santi, Natalí Soler Matubaro ddc 530 bkl 33.00 misc Black hole thermodynamics misc Black hole evaporation misc Mass evolution of black holes misc Schwarzschild black hole Mass Evolution of Schwarzschild Black Holes
authorStr	de Santi, Natalí Soler Matubaro
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topic_title	530 ASE 33.00 bkl Mass Evolution of Schwarzschild Black Holes Black hole thermodynamics (dpeaa)DE-He213 Black hole evaporation (dpeaa)DE-He213 Mass evolution of black holes (dpeaa)DE-He213 Schwarzschild black hole (dpeaa)DE-He213
topic	ddc 530 bkl 33.00 misc Black hole thermodynamics misc Black hole evaporation misc Mass evolution of black holes misc Schwarzschild black hole
topic_unstemmed	ddc 530 bkl 33.00 misc Black hole thermodynamics misc Black hole evaporation misc Mass evolution of black holes misc Schwarzschild black hole
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title	Mass Evolution of Schwarzschild Black Holes
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title_full	Mass Evolution of Schwarzschild Black Holes
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title_sort	mass evolution of schwarzschild black holes
title_auth	Mass Evolution of Schwarzschild Black Holes
abstract	Abstract In the classical theory of general relativity, black holes can only absorb and not emit particles. When quantum mechanical effects are taken into account, then the black holes emit particles as hot bodies with temperature proportional to κ, its surface gravity. This thermal emission can lead to a slow decrease in the mass of the black hole, and eventually to its disappearance, also called black hole evaporation. This characteristic allows us to analyze what happens with the mass of the black hole when its temperature is increased or decreased and how the energy is exchanged with the external environment. This paper has the aim to make a discussion about the mass evolution, due to Hawking radiation emission, of Schwarzschild black holes with different initial masses and external conditions as the empty space, the cosmic microwave background with constant temperature, and with temperature varying in accordance with the eras of the universe. Our main contributions are to take into account these variations in the temperature of the cosmic background radiation and use them into the black holes dynamics and also to analyze the asymptotic behavior of the solutions. As a result, we have the complete evaporation of the black holes in most cases, although their masses can increase in some cases, and even diverge for specific conditions.
abstractGer	Abstract In the classical theory of general relativity, black holes can only absorb and not emit particles. When quantum mechanical effects are taken into account, then the black holes emit particles as hot bodies with temperature proportional to κ, its surface gravity. This thermal emission can lead to a slow decrease in the mass of the black hole, and eventually to its disappearance, also called black hole evaporation. This characteristic allows us to analyze what happens with the mass of the black hole when its temperature is increased or decreased and how the energy is exchanged with the external environment. This paper has the aim to make a discussion about the mass evolution, due to Hawking radiation emission, of Schwarzschild black holes with different initial masses and external conditions as the empty space, the cosmic microwave background with constant temperature, and with temperature varying in accordance with the eras of the universe. Our main contributions are to take into account these variations in the temperature of the cosmic background radiation and use them into the black holes dynamics and also to analyze the asymptotic behavior of the solutions. As a result, we have the complete evaporation of the black holes in most cases, although their masses can increase in some cases, and even diverge for specific conditions.
abstract_unstemmed	Abstract In the classical theory of general relativity, black holes can only absorb and not emit particles. When quantum mechanical effects are taken into account, then the black holes emit particles as hot bodies with temperature proportional to κ, its surface gravity. This thermal emission can lead to a slow decrease in the mass of the black hole, and eventually to its disappearance, also called black hole evaporation. This characteristic allows us to analyze what happens with the mass of the black hole when its temperature is increased or decreased and how the energy is exchanged with the external environment. This paper has the aim to make a discussion about the mass evolution, due to Hawking radiation emission, of Schwarzschild black holes with different initial masses and external conditions as the empty space, the cosmic microwave background with constant temperature, and with temperature varying in accordance with the eras of the universe. Our main contributions are to take into account these variations in the temperature of the cosmic background radiation and use them into the black holes dynamics and also to analyze the asymptotic behavior of the solutions. As a result, we have the complete evaporation of the black holes in most cases, although their masses can increase in some cases, and even diverge for specific conditions.
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container_issue	6
title_short	Mass Evolution of Schwarzschild Black Holes
url	https://dx.doi.org/10.1007/s13538-019-00708-y
remote_bool	true
author2	Santarelli, Raphael
author2Str	Santarelli, Raphael
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doi_str	10.1007/s13538-019-00708-y
up_date	2024-07-04T01:06:07.412Z
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score	7.399001

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Mass Evolution of Schwarzschild Black Holes

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