Positron annihilation signatures associated with the outburst of the microquasar V404 Cygni

Microquasars1-4 are stellar-mass black holes accreting matter from a companion star5 and ejecting plasma jets at almost the speed of light. They are analogues of quasars that contain supermassive black holes of 10^sup 6^ to 10^sup 10^ solar masses. Accretion in microquasars varies on much shorter ti...
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Gespeichert in:

Autor*in:	Thomas Siegert [verfasserIn] Roland Diehl Jochen Greiner Martin G H Krause Andrei M Beloborodov Marion Cadolle Bel Fabrizia Guglielmetti Jerome Rodriguez Andrew W Strong Xiaoling Zhang

Format:	Artikel
Sprache:	Englisch

Erschienen:	2016

Schlagwörter:	Black holes Stars & galaxies Magnetic fields Plasma Quasars Positrons Positron annihilation Black holes (Astronomy) Stars, Double Analysis High Energy Astrophysical Phenomena Astrophysics

Übergeordnetes Werk:	Enthalten in: Nature - London : Macmillan Publishers Limited, part of Springer Nature, 1869, 531(2016), 7594, Seite 341-343
Übergeordnetes Werk:	volume:531 ; year:2016 ; number:7594 ; pages:341-343

Links:	Volltext Link aufrufen Link aufrufen Link aufrufen

DOI / URN:	10.1038/nature16978

Katalog-ID:	OLC1972873458

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publishDate	2016
allfields	10.1038/nature16978 doi PQ20160430 (DE-627)OLC1972873458 (DE-599)GBVOLC1972873458 (PRQ)a2426-daf9d3a1cfa132cfac96908680c14e4bd59c7f3465ad0e63bb6e9876953e388e0 (KEY)0072945020160000531759400341positronannihilationsignaturesassociatedwiththeout DE-627 ger DE-627 rakwb eng 070 500 DNB 500 AVZ BIODIV fid Thomas Siegert verfasserin aut Positron annihilation signatures associated with the outburst of the microquasar V404 Cygni 2016 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier Microquasars1-4 are stellar-mass black holes accreting matter from a companion star5 and ejecting plasma jets at almost the speed of light. They are analogues of quasars that contain supermassive black holes of 10^sup 6^ to 10^sup 10^ solar masses. Accretion in microquasars varies on much shorter timescales than in quasars and occasionally produces exceptionally bright X-ray flares6. How the flares are produced is unclear, as is the mechanism for launching the relativistic jets and their composition. An emission line near 511 kiloelectronvolts has long been sought in the emission spectrum of microquasars as evidence for the expected electron- positron plasma. Transient high-energy spectral features have been reported in two objects7,8, but their positron interpretation9 remains contentious. Here we report observations of γ-ray emission from the microquasar V404 Cygni during a recent period of strong flaring activity10. The emission spectrum around 511 kiloelectronvolts shows clear signatures of variable positron annihilation, which implies a high rate of positron production. This supports the earlier conjecture that microquasars may be the main sources of the electron-positron plasma responsible for the bright diffuse emission of annihilation γ-rays in the bulge region of our Galaxy11. Additionally, microquasars could be the origin of the observed megaelectronvolt continuum excess in the inner Galaxy. Black holes Stars & galaxies Magnetic fields Plasma Quasars Positrons Positron annihilation Black holes (Astronomy) Stars, Double Analysis High Energy Astrophysical Phenomena Astrophysics Roland Diehl oth Jochen Greiner oth Martin G H Krause oth Andrei M Beloborodov oth Marion Cadolle Bel oth Fabrizia Guglielmetti oth Jerome Rodriguez oth Andrew W Strong oth Xiaoling Zhang oth Enthalten in Nature London : Macmillan Publishers Limited, part of Springer Nature, 1869 531(2016), 7594, Seite 341-343 (DE-627)129292834 (DE-600)120714-3 (DE-576)014473941 0028-0836 nnns volume:531 year:2016 number:7594 pages:341-343 http://dx.doi.org/10.1038/nature16978 Volltext http://www.ncbi.nlm.nih.gov/pubmed/26934231 http://search.proquest.com/docview/1774914633 http://arxiv.org/abs/1603.01169 GBV_USEFLAG_A SYSFLAG_A GBV_OLC FID-BIODIV SSG-OLC-PHY SSG-OLC-CHE SSG-OLC-MAT SSG-OLC-FOR SSG-OLC-SPO SSG-OLC-PHA SSG-OLC-DE-84 SSG-OPC-FOR GBV_ILN_11 GBV_ILN_22 GBV_ILN_30 GBV_ILN_40 GBV_ILN_47 GBV_ILN_55 GBV_ILN_59 GBV_ILN_60 GBV_ILN_62 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_101 GBV_ILN_110 GBV_ILN_120 GBV_ILN_154 GBV_ILN_168 GBV_ILN_170 GBV_ILN_171 GBV_ILN_211 GBV_ILN_290 GBV_ILN_294 GBV_ILN_601 GBV_ILN_647 GBV_ILN_754 GBV_ILN_2001 GBV_ILN_2002 GBV_ILN_2003 GBV_ILN_2005 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2015 GBV_ILN_2016 GBV_ILN_2018 GBV_ILN_2020 GBV_ILN_2026 GBV_ILN_2095 GBV_ILN_2116 GBV_ILN_2120 GBV_ILN_2121 GBV_ILN_2219 GBV_ILN_2221 GBV_ILN_2279 GBV_ILN_2286 GBV_ILN_4012 GBV_ILN_4035 GBV_ILN_4125 GBV_ILN_4219 GBV_ILN_4251 GBV_ILN_4277 GBV_ILN_4302 GBV_ILN_4305 GBV_ILN_4313 GBV_ILN_4314 GBV_ILN_4317 GBV_ILN_4320 GBV_ILN_4324 GBV_ILN_4700 AR 531 2016 7594 341-343
spelling	10.1038/nature16978 doi PQ20160430 (DE-627)OLC1972873458 (DE-599)GBVOLC1972873458 (PRQ)a2426-daf9d3a1cfa132cfac96908680c14e4bd59c7f3465ad0e63bb6e9876953e388e0 (KEY)0072945020160000531759400341positronannihilationsignaturesassociatedwiththeout DE-627 ger DE-627 rakwb eng 070 500 DNB 500 AVZ BIODIV fid Thomas Siegert verfasserin aut Positron annihilation signatures associated with the outburst of the microquasar V404 Cygni 2016 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier Microquasars1-4 are stellar-mass black holes accreting matter from a companion star5 and ejecting plasma jets at almost the speed of light. They are analogues of quasars that contain supermassive black holes of 10^sup 6^ to 10^sup 10^ solar masses. Accretion in microquasars varies on much shorter timescales than in quasars and occasionally produces exceptionally bright X-ray flares6. How the flares are produced is unclear, as is the mechanism for launching the relativistic jets and their composition. An emission line near 511 kiloelectronvolts has long been sought in the emission spectrum of microquasars as evidence for the expected electron- positron plasma. Transient high-energy spectral features have been reported in two objects7,8, but their positron interpretation9 remains contentious. Here we report observations of γ-ray emission from the microquasar V404 Cygni during a recent period of strong flaring activity10. The emission spectrum around 511 kiloelectronvolts shows clear signatures of variable positron annihilation, which implies a high rate of positron production. This supports the earlier conjecture that microquasars may be the main sources of the electron-positron plasma responsible for the bright diffuse emission of annihilation γ-rays in the bulge region of our Galaxy11. Additionally, microquasars could be the origin of the observed megaelectronvolt continuum excess in the inner Galaxy. Black holes Stars & galaxies Magnetic fields Plasma Quasars Positrons Positron annihilation Black holes (Astronomy) Stars, Double Analysis High Energy Astrophysical Phenomena Astrophysics Roland Diehl oth Jochen Greiner oth Martin G H Krause oth Andrei M Beloborodov oth Marion Cadolle Bel oth Fabrizia Guglielmetti oth Jerome Rodriguez oth Andrew W Strong oth Xiaoling Zhang oth Enthalten in Nature London : Macmillan Publishers Limited, part of Springer Nature, 1869 531(2016), 7594, Seite 341-343 (DE-627)129292834 (DE-600)120714-3 (DE-576)014473941 0028-0836 nnns volume:531 year:2016 number:7594 pages:341-343 http://dx.doi.org/10.1038/nature16978 Volltext http://www.ncbi.nlm.nih.gov/pubmed/26934231 http://search.proquest.com/docview/1774914633 http://arxiv.org/abs/1603.01169 GBV_USEFLAG_A SYSFLAG_A GBV_OLC FID-BIODIV SSG-OLC-PHY SSG-OLC-CHE SSG-OLC-MAT SSG-OLC-FOR SSG-OLC-SPO SSG-OLC-PHA SSG-OLC-DE-84 SSG-OPC-FOR GBV_ILN_11 GBV_ILN_22 GBV_ILN_30 GBV_ILN_40 GBV_ILN_47 GBV_ILN_55 GBV_ILN_59 GBV_ILN_60 GBV_ILN_62 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_101 GBV_ILN_110 GBV_ILN_120 GBV_ILN_154 GBV_ILN_168 GBV_ILN_170 GBV_ILN_171 GBV_ILN_211 GBV_ILN_290 GBV_ILN_294 GBV_ILN_601 GBV_ILN_647 GBV_ILN_754 GBV_ILN_2001 GBV_ILN_2002 GBV_ILN_2003 GBV_ILN_2005 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2015 GBV_ILN_2016 GBV_ILN_2018 GBV_ILN_2020 GBV_ILN_2026 GBV_ILN_2095 GBV_ILN_2116 GBV_ILN_2120 GBV_ILN_2121 GBV_ILN_2219 GBV_ILN_2221 GBV_ILN_2279 GBV_ILN_2286 GBV_ILN_4012 GBV_ILN_4035 GBV_ILN_4125 GBV_ILN_4219 GBV_ILN_4251 GBV_ILN_4277 GBV_ILN_4302 GBV_ILN_4305 GBV_ILN_4313 GBV_ILN_4314 GBV_ILN_4317 GBV_ILN_4320 GBV_ILN_4324 GBV_ILN_4700 AR 531 2016 7594 341-343
allfields_unstemmed	10.1038/nature16978 doi PQ20160430 (DE-627)OLC1972873458 (DE-599)GBVOLC1972873458 (PRQ)a2426-daf9d3a1cfa132cfac96908680c14e4bd59c7f3465ad0e63bb6e9876953e388e0 (KEY)0072945020160000531759400341positronannihilationsignaturesassociatedwiththeout DE-627 ger DE-627 rakwb eng 070 500 DNB 500 AVZ BIODIV fid Thomas Siegert verfasserin aut Positron annihilation signatures associated with the outburst of the microquasar V404 Cygni 2016 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier Microquasars1-4 are stellar-mass black holes accreting matter from a companion star5 and ejecting plasma jets at almost the speed of light. They are analogues of quasars that contain supermassive black holes of 10^sup 6^ to 10^sup 10^ solar masses. Accretion in microquasars varies on much shorter timescales than in quasars and occasionally produces exceptionally bright X-ray flares6. How the flares are produced is unclear, as is the mechanism for launching the relativistic jets and their composition. An emission line near 511 kiloelectronvolts has long been sought in the emission spectrum of microquasars as evidence for the expected electron- positron plasma. Transient high-energy spectral features have been reported in two objects7,8, but their positron interpretation9 remains contentious. Here we report observations of γ-ray emission from the microquasar V404 Cygni during a recent period of strong flaring activity10. The emission spectrum around 511 kiloelectronvolts shows clear signatures of variable positron annihilation, which implies a high rate of positron production. This supports the earlier conjecture that microquasars may be the main sources of the electron-positron plasma responsible for the bright diffuse emission of annihilation γ-rays in the bulge region of our Galaxy11. Additionally, microquasars could be the origin of the observed megaelectronvolt continuum excess in the inner Galaxy. Black holes Stars & galaxies Magnetic fields Plasma Quasars Positrons Positron annihilation Black holes (Astronomy) Stars, Double Analysis High Energy Astrophysical Phenomena Astrophysics Roland Diehl oth Jochen Greiner oth Martin G H Krause oth Andrei M Beloborodov oth Marion Cadolle Bel oth Fabrizia Guglielmetti oth Jerome Rodriguez oth Andrew W Strong oth Xiaoling Zhang oth Enthalten in Nature London : Macmillan Publishers Limited, part of Springer Nature, 1869 531(2016), 7594, Seite 341-343 (DE-627)129292834 (DE-600)120714-3 (DE-576)014473941 0028-0836 nnns volume:531 year:2016 number:7594 pages:341-343 http://dx.doi.org/10.1038/nature16978 Volltext http://www.ncbi.nlm.nih.gov/pubmed/26934231 http://search.proquest.com/docview/1774914633 http://arxiv.org/abs/1603.01169 GBV_USEFLAG_A SYSFLAG_A GBV_OLC FID-BIODIV SSG-OLC-PHY SSG-OLC-CHE SSG-OLC-MAT SSG-OLC-FOR SSG-OLC-SPO SSG-OLC-PHA SSG-OLC-DE-84 SSG-OPC-FOR GBV_ILN_11 GBV_ILN_22 GBV_ILN_30 GBV_ILN_40 GBV_ILN_47 GBV_ILN_55 GBV_ILN_59 GBV_ILN_60 GBV_ILN_62 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_101 GBV_ILN_110 GBV_ILN_120 GBV_ILN_154 GBV_ILN_168 GBV_ILN_170 GBV_ILN_171 GBV_ILN_211 GBV_ILN_290 GBV_ILN_294 GBV_ILN_601 GBV_ILN_647 GBV_ILN_754 GBV_ILN_2001 GBV_ILN_2002 GBV_ILN_2003 GBV_ILN_2005 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2015 GBV_ILN_2016 GBV_ILN_2018 GBV_ILN_2020 GBV_ILN_2026 GBV_ILN_2095 GBV_ILN_2116 GBV_ILN_2120 GBV_ILN_2121 GBV_ILN_2219 GBV_ILN_2221 GBV_ILN_2279 GBV_ILN_2286 GBV_ILN_4012 GBV_ILN_4035 GBV_ILN_4125 GBV_ILN_4219 GBV_ILN_4251 GBV_ILN_4277 GBV_ILN_4302 GBV_ILN_4305 GBV_ILN_4313 GBV_ILN_4314 GBV_ILN_4317 GBV_ILN_4320 GBV_ILN_4324 GBV_ILN_4700 AR 531 2016 7594 341-343
allfieldsGer	10.1038/nature16978 doi PQ20160430 (DE-627)OLC1972873458 (DE-599)GBVOLC1972873458 (PRQ)a2426-daf9d3a1cfa132cfac96908680c14e4bd59c7f3465ad0e63bb6e9876953e388e0 (KEY)0072945020160000531759400341positronannihilationsignaturesassociatedwiththeout DE-627 ger DE-627 rakwb eng 070 500 DNB 500 AVZ BIODIV fid Thomas Siegert verfasserin aut Positron annihilation signatures associated with the outburst of the microquasar V404 Cygni 2016 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier Microquasars1-4 are stellar-mass black holes accreting matter from a companion star5 and ejecting plasma jets at almost the speed of light. They are analogues of quasars that contain supermassive black holes of 10^sup 6^ to 10^sup 10^ solar masses. Accretion in microquasars varies on much shorter timescales than in quasars and occasionally produces exceptionally bright X-ray flares6. How the flares are produced is unclear, as is the mechanism for launching the relativistic jets and their composition. An emission line near 511 kiloelectronvolts has long been sought in the emission spectrum of microquasars as evidence for the expected electron- positron plasma. Transient high-energy spectral features have been reported in two objects7,8, but their positron interpretation9 remains contentious. Here we report observations of γ-ray emission from the microquasar V404 Cygni during a recent period of strong flaring activity10. The emission spectrum around 511 kiloelectronvolts shows clear signatures of variable positron annihilation, which implies a high rate of positron production. This supports the earlier conjecture that microquasars may be the main sources of the electron-positron plasma responsible for the bright diffuse emission of annihilation γ-rays in the bulge region of our Galaxy11. Additionally, microquasars could be the origin of the observed megaelectronvolt continuum excess in the inner Galaxy. Black holes Stars & galaxies Magnetic fields Plasma Quasars Positrons Positron annihilation Black holes (Astronomy) Stars, Double Analysis High Energy Astrophysical Phenomena Astrophysics Roland Diehl oth Jochen Greiner oth Martin G H Krause oth Andrei M Beloborodov oth Marion Cadolle Bel oth Fabrizia Guglielmetti oth Jerome Rodriguez oth Andrew W Strong oth Xiaoling Zhang oth Enthalten in Nature London : Macmillan Publishers Limited, part of Springer Nature, 1869 531(2016), 7594, Seite 341-343 (DE-627)129292834 (DE-600)120714-3 (DE-576)014473941 0028-0836 nnns volume:531 year:2016 number:7594 pages:341-343 http://dx.doi.org/10.1038/nature16978 Volltext http://www.ncbi.nlm.nih.gov/pubmed/26934231 http://search.proquest.com/docview/1774914633 http://arxiv.org/abs/1603.01169 GBV_USEFLAG_A SYSFLAG_A GBV_OLC FID-BIODIV SSG-OLC-PHY SSG-OLC-CHE SSG-OLC-MAT SSG-OLC-FOR SSG-OLC-SPO SSG-OLC-PHA SSG-OLC-DE-84 SSG-OPC-FOR GBV_ILN_11 GBV_ILN_22 GBV_ILN_30 GBV_ILN_40 GBV_ILN_47 GBV_ILN_55 GBV_ILN_59 GBV_ILN_60 GBV_ILN_62 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_101 GBV_ILN_110 GBV_ILN_120 GBV_ILN_154 GBV_ILN_168 GBV_ILN_170 GBV_ILN_171 GBV_ILN_211 GBV_ILN_290 GBV_ILN_294 GBV_ILN_601 GBV_ILN_647 GBV_ILN_754 GBV_ILN_2001 GBV_ILN_2002 GBV_ILN_2003 GBV_ILN_2005 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2015 GBV_ILN_2016 GBV_ILN_2018 GBV_ILN_2020 GBV_ILN_2026 GBV_ILN_2095 GBV_ILN_2116 GBV_ILN_2120 GBV_ILN_2121 GBV_ILN_2219 GBV_ILN_2221 GBV_ILN_2279 GBV_ILN_2286 GBV_ILN_4012 GBV_ILN_4035 GBV_ILN_4125 GBV_ILN_4219 GBV_ILN_4251 GBV_ILN_4277 GBV_ILN_4302 GBV_ILN_4305 GBV_ILN_4313 GBV_ILN_4314 GBV_ILN_4317 GBV_ILN_4320 GBV_ILN_4324 GBV_ILN_4700 AR 531 2016 7594 341-343
allfieldsSound	10.1038/nature16978 doi PQ20160430 (DE-627)OLC1972873458 (DE-599)GBVOLC1972873458 (PRQ)a2426-daf9d3a1cfa132cfac96908680c14e4bd59c7f3465ad0e63bb6e9876953e388e0 (KEY)0072945020160000531759400341positronannihilationsignaturesassociatedwiththeout DE-627 ger DE-627 rakwb eng 070 500 DNB 500 AVZ BIODIV fid Thomas Siegert verfasserin aut Positron annihilation signatures associated with the outburst of the microquasar V404 Cygni 2016 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier Microquasars1-4 are stellar-mass black holes accreting matter from a companion star5 and ejecting plasma jets at almost the speed of light. They are analogues of quasars that contain supermassive black holes of 10^sup 6^ to 10^sup 10^ solar masses. Accretion in microquasars varies on much shorter timescales than in quasars and occasionally produces exceptionally bright X-ray flares6. How the flares are produced is unclear, as is the mechanism for launching the relativistic jets and their composition. An emission line near 511 kiloelectronvolts has long been sought in the emission spectrum of microquasars as evidence for the expected electron- positron plasma. Transient high-energy spectral features have been reported in two objects7,8, but their positron interpretation9 remains contentious. Here we report observations of γ-ray emission from the microquasar V404 Cygni during a recent period of strong flaring activity10. The emission spectrum around 511 kiloelectronvolts shows clear signatures of variable positron annihilation, which implies a high rate of positron production. This supports the earlier conjecture that microquasars may be the main sources of the electron-positron plasma responsible for the bright diffuse emission of annihilation γ-rays in the bulge region of our Galaxy11. Additionally, microquasars could be the origin of the observed megaelectronvolt continuum excess in the inner Galaxy. Black holes Stars & galaxies Magnetic fields Plasma Quasars Positrons Positron annihilation Black holes (Astronomy) Stars, Double Analysis High Energy Astrophysical Phenomena Astrophysics Roland Diehl oth Jochen Greiner oth Martin G H Krause oth Andrei M Beloborodov oth Marion Cadolle Bel oth Fabrizia Guglielmetti oth Jerome Rodriguez oth Andrew W Strong oth Xiaoling Zhang oth Enthalten in Nature London : Macmillan Publishers Limited, part of Springer Nature, 1869 531(2016), 7594, Seite 341-343 (DE-627)129292834 (DE-600)120714-3 (DE-576)014473941 0028-0836 nnns volume:531 year:2016 number:7594 pages:341-343 http://dx.doi.org/10.1038/nature16978 Volltext http://www.ncbi.nlm.nih.gov/pubmed/26934231 http://search.proquest.com/docview/1774914633 http://arxiv.org/abs/1603.01169 GBV_USEFLAG_A SYSFLAG_A GBV_OLC FID-BIODIV SSG-OLC-PHY SSG-OLC-CHE SSG-OLC-MAT SSG-OLC-FOR SSG-OLC-SPO SSG-OLC-PHA SSG-OLC-DE-84 SSG-OPC-FOR GBV_ILN_11 GBV_ILN_22 GBV_ILN_30 GBV_ILN_40 GBV_ILN_47 GBV_ILN_55 GBV_ILN_59 GBV_ILN_60 GBV_ILN_62 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_101 GBV_ILN_110 GBV_ILN_120 GBV_ILN_154 GBV_ILN_168 GBV_ILN_170 GBV_ILN_171 GBV_ILN_211 GBV_ILN_290 GBV_ILN_294 GBV_ILN_601 GBV_ILN_647 GBV_ILN_754 GBV_ILN_2001 GBV_ILN_2002 GBV_ILN_2003 GBV_ILN_2005 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2015 GBV_ILN_2016 GBV_ILN_2018 GBV_ILN_2020 GBV_ILN_2026 GBV_ILN_2095 GBV_ILN_2116 GBV_ILN_2120 GBV_ILN_2121 GBV_ILN_2219 GBV_ILN_2221 GBV_ILN_2279 GBV_ILN_2286 GBV_ILN_4012 GBV_ILN_4035 GBV_ILN_4125 GBV_ILN_4219 GBV_ILN_4251 GBV_ILN_4277 GBV_ILN_4302 GBV_ILN_4305 GBV_ILN_4313 GBV_ILN_4314 GBV_ILN_4317 GBV_ILN_4320 GBV_ILN_4324 GBV_ILN_4700 AR 531 2016 7594 341-343
language	English
source	Enthalten in Nature 531(2016), 7594, Seite 341-343 volume:531 year:2016 number:7594 pages:341-343
sourceStr	Enthalten in Nature 531(2016), 7594, Seite 341-343 volume:531 year:2016 number:7594 pages:341-343
format_phy_str_mv	Article
institution	findex.gbv.de
topic_facet	Black holes Stars & galaxies Magnetic fields Plasma Quasars Positrons Positron annihilation Black holes (Astronomy) Stars, Double Analysis High Energy Astrophysical Phenomena Astrophysics
dewey-raw	070
isfreeaccess_bool	false
container_title	Nature
authorswithroles_txt_mv	Thomas Siegert @@aut@@ Roland Diehl @@oth@@ Jochen Greiner @@oth@@ Martin G H Krause @@oth@@ Andrei M Beloborodov @@oth@@ Marion Cadolle Bel @@oth@@ Fabrizia Guglielmetti @@oth@@ Jerome Rodriguez @@oth@@ Andrew W Strong @@oth@@ Xiaoling Zhang @@oth@@
publishDateDaySort_date	2016-01-01T00:00:00Z
hierarchy_top_id	129292834
dewey-sort	270
id	OLC1972873458
language_de	englisch
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author	Thomas Siegert
spellingShingle	Thomas Siegert ddc 070 ddc 500 fid BIODIV misc Black holes misc Stars & galaxies misc Magnetic fields misc Plasma misc Quasars misc Positrons misc Positron annihilation misc Black holes (Astronomy) misc Stars, Double misc Analysis misc High Energy Astrophysical Phenomena misc Astrophysics Positron annihilation signatures associated with the outburst of the microquasar V404 Cygni
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topic_title	070 500 DNB 500 AVZ BIODIV fid Positron annihilation signatures associated with the outburst of the microquasar V404 Cygni Black holes Stars & galaxies Magnetic fields Plasma Quasars Positrons Positron annihilation Black holes (Astronomy) Stars, Double Analysis High Energy Astrophysical Phenomena Astrophysics
topic	ddc 070 ddc 500 fid BIODIV misc Black holes misc Stars & galaxies misc Magnetic fields misc Plasma misc Quasars misc Positrons misc Positron annihilation misc Black holes (Astronomy) misc Stars, Double misc Analysis misc High Energy Astrophysical Phenomena misc Astrophysics
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title	Positron annihilation signatures associated with the outburst of the microquasar V404 Cygni
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title_full	Positron annihilation signatures associated with the outburst of the microquasar V404 Cygni
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title_sort	positron annihilation signatures associated with the outburst of the microquasar v404 cygni
title_auth	Positron annihilation signatures associated with the outburst of the microquasar V404 Cygni
abstract	Microquasars1-4 are stellar-mass black holes accreting matter from a companion star5 and ejecting plasma jets at almost the speed of light. They are analogues of quasars that contain supermassive black holes of 10^sup 6^ to 10^sup 10^ solar masses. Accretion in microquasars varies on much shorter timescales than in quasars and occasionally produces exceptionally bright X-ray flares6. How the flares are produced is unclear, as is the mechanism for launching the relativistic jets and their composition. An emission line near 511 kiloelectronvolts has long been sought in the emission spectrum of microquasars as evidence for the expected electron- positron plasma. Transient high-energy spectral features have been reported in two objects7,8, but their positron interpretation9 remains contentious. Here we report observations of γ-ray emission from the microquasar V404 Cygni during a recent period of strong flaring activity10. The emission spectrum around 511 kiloelectronvolts shows clear signatures of variable positron annihilation, which implies a high rate of positron production. This supports the earlier conjecture that microquasars may be the main sources of the electron-positron plasma responsible for the bright diffuse emission of annihilation γ-rays in the bulge region of our Galaxy11. Additionally, microquasars could be the origin of the observed megaelectronvolt continuum excess in the inner Galaxy.
abstractGer	Microquasars1-4 are stellar-mass black holes accreting matter from a companion star5 and ejecting plasma jets at almost the speed of light. They are analogues of quasars that contain supermassive black holes of 10^sup 6^ to 10^sup 10^ solar masses. Accretion in microquasars varies on much shorter timescales than in quasars and occasionally produces exceptionally bright X-ray flares6. How the flares are produced is unclear, as is the mechanism for launching the relativistic jets and their composition. An emission line near 511 kiloelectronvolts has long been sought in the emission spectrum of microquasars as evidence for the expected electron- positron plasma. Transient high-energy spectral features have been reported in two objects7,8, but their positron interpretation9 remains contentious. Here we report observations of γ-ray emission from the microquasar V404 Cygni during a recent period of strong flaring activity10. The emission spectrum around 511 kiloelectronvolts shows clear signatures of variable positron annihilation, which implies a high rate of positron production. This supports the earlier conjecture that microquasars may be the main sources of the electron-positron plasma responsible for the bright diffuse emission of annihilation γ-rays in the bulge region of our Galaxy11. Additionally, microquasars could be the origin of the observed megaelectronvolt continuum excess in the inner Galaxy.
abstract_unstemmed	Microquasars1-4 are stellar-mass black holes accreting matter from a companion star5 and ejecting plasma jets at almost the speed of light. They are analogues of quasars that contain supermassive black holes of 10^sup 6^ to 10^sup 10^ solar masses. Accretion in microquasars varies on much shorter timescales than in quasars and occasionally produces exceptionally bright X-ray flares6. How the flares are produced is unclear, as is the mechanism for launching the relativistic jets and their composition. An emission line near 511 kiloelectronvolts has long been sought in the emission spectrum of microquasars as evidence for the expected electron- positron plasma. Transient high-energy spectral features have been reported in two objects7,8, but their positron interpretation9 remains contentious. Here we report observations of γ-ray emission from the microquasar V404 Cygni during a recent period of strong flaring activity10. The emission spectrum around 511 kiloelectronvolts shows clear signatures of variable positron annihilation, which implies a high rate of positron production. This supports the earlier conjecture that microquasars may be the main sources of the electron-positron plasma responsible for the bright diffuse emission of annihilation γ-rays in the bulge region of our Galaxy11. Additionally, microquasars could be the origin of the observed megaelectronvolt continuum excess in the inner Galaxy.
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container_issue	7594
title_short	Positron annihilation signatures associated with the outburst of the microquasar V404 Cygni
url	http://dx.doi.org/10.1038/nature16978 http://www.ncbi.nlm.nih.gov/pubmed/26934231 http://search.proquest.com/docview/1774914633 http://arxiv.org/abs/1603.01169
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author2	Roland Diehl Jochen Greiner Martin G H Krause Andrei M Beloborodov Marion Cadolle Bel Fabrizia Guglielmetti Jerome Rodriguez Andrew W Strong Xiaoling Zhang
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Positron annihilation signatures associated with the outburst of the microquasar V404 Cygni

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Vorhandene Bände

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