The awakening of a classical nova from hibernation

Cataclysmic variable stars-novae, dwarf novae, and nova-likes-are close binary systems consisting of a white dwarf star (the primary) that is accreting matter from a low-mass companion star (the secondary)1. From time to time such systems undergo large-amplitude brightenings. The most spectacular eruptions, with a ten-thousandfold increase in brightness, occur in classical novae and are caused by a thermonuclear runaway on the surface of the white dwarf2. Such eruptions are thought to recur on timescales of ten thousand to a million years3. In between, the system's properties depend primarily on the mass-transfer rate: if it is lower than a billionth of a solar mass per year, the accretion becomes unstable and the matter is dumped onto the white dwarf during quasi-periodic dwarf nova outbursts4. The hibernation hypothesis5 predicts that nova eruptions strongly affect the mass-transfer rate in the binary, keeping it high for centuries after the event6. Subsequently, the mass-transfer rate should significantly decrease for a thousand to a million years, starting the hibernation phase. After that the nova awakes again-with accretion returning to the pre-eruption level and leading to a new nova explosion. The hibernation model predicts cyclical evolution of cataclysmic variables through phases of high and low mass-transfer. The theory gained some support from the discovery of ancient nova shells around the dwarf novae Z Camelopardalis7 and AT Cancri8, but direct evidence for considerable mass-transfer changes prior, during and after nova eruptions has not hitherto been found. Here we report long-term observations of the classical nova V1213 Cen (Nova Centauri 2009) covering its pre- and post-eruption phases and precisely documenting its evolution. Within the six years before the explosion, the system revealed dwarf nova outbursts indicative of a low mass-transfer rate. The post-nova is two orders of magnitude brighter than the pre-nova at minimum light with no trace of dwarf nova behaviour, implying that the mass-transfer rate increased considerably as a result of the nova explosion. Ausführliche Beschreibung

Gespeichert in:

Autor*in:	Przemek Mróz [verfasserIn] Andrzej Udalski Pawel Pietrukowicz Michal K Szymanski Igor Soszynski Lukasz Wyrzykowski Radoslaw Poleski Szymon Kozlowski Jan Skowron Krzysztof Ulaczyk Dorota Skowron Michal Pawlak

Format:	Artikel
Sprache:	Englisch

Erschienen:	2016

Schlagwörter:	White dwarfs Astronomy Accretion disks Observations Stars, New Solar and Stellar Astrophysics Astrophysics

Übergeordnetes Werk:	Enthalten in: Nature - London : Macmillan Publishers Limited, part of Springer Nature, 1869, 537(2016), 7622, Seite 649-651
Übergeordnetes Werk:	volume:537 ; year:2016 ; number:7622 ; pages:649-651

Links:	Volltext Link aufrufen Link aufrufen

DOI / URN:	10.1038/nature19066

Katalog-ID:	OLC1982122110

Internformat


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700	0		\|a Szymon Kozlowski \|4 oth
700	0		\|a Jan Skowron \|4 oth
700	0		\|a Krzysztof Ulaczyk \|4 oth
700	0		\|a Dorota Skowron \|4 oth
700	0		\|a Michal Pawlak \|4 oth
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publishDate	2016
allfields	10.1038/nature19066 doi PQ20170206 (DE-627)OLC1982122110 (DE-599)GBVOLC1982122110 (PRQ)a2081-a34e864c1852087018682baf039cdee6ef82fcaeccef5286a160f3f785cd077c0 (KEY)0072945020160000537762200649awakeningofaclassicalnovafromhibernation DE-627 ger DE-627 rakwb eng 070 500 DE-101 500 AVZ BIODIV fid Przemek Mróz verfasserin aut The awakening of a classical nova from hibernation 2016 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier Cataclysmic variable stars-novae, dwarf novae, and nova-likes-are close binary systems consisting of a white dwarf star (the primary) that is accreting matter from a low-mass companion star (the secondary)1. From time to time such systems undergo large-amplitude brightenings. The most spectacular eruptions, with a ten-thousandfold increase in brightness, occur in classical novae and are caused by a thermonuclear runaway on the surface of the white dwarf2. Such eruptions are thought to recur on timescales of ten thousand to a million years3. In between, the system's properties depend primarily on the mass-transfer rate: if it is lower than a billionth of a solar mass per year, the accretion becomes unstable and the matter is dumped onto the white dwarf during quasi-periodic dwarf nova outbursts4. The hibernation hypothesis5 predicts that nova eruptions strongly affect the mass-transfer rate in the binary, keeping it high for centuries after the event6. Subsequently, the mass-transfer rate should significantly decrease for a thousand to a million years, starting the hibernation phase. After that the nova awakes again-with accretion returning to the pre-eruption level and leading to a new nova explosion. The hibernation model predicts cyclical evolution of cataclysmic variables through phases of high and low mass-transfer. The theory gained some support from the discovery of ancient nova shells around the dwarf novae Z Camelopardalis7 and AT Cancri8, but direct evidence for considerable mass-transfer changes prior, during and after nova eruptions has not hitherto been found. Here we report long-term observations of the classical nova V1213 Cen (Nova Centauri 2009) covering its pre- and post-eruption phases and precisely documenting its evolution. Within the six years before the explosion, the system revealed dwarf nova outbursts indicative of a low mass-transfer rate. The post-nova is two orders of magnitude brighter than the pre-nova at minimum light with no trace of dwarf nova behaviour, implying that the mass-transfer rate increased considerably as a result of the nova explosion. White dwarfs Astronomy Accretion disks Observations Stars, New Solar and Stellar Astrophysics Astrophysics Andrzej Udalski oth Pawel Pietrukowicz oth Michal K Szymanski oth Igor Soszynski oth Lukasz Wyrzykowski oth Radoslaw Poleski oth Szymon Kozlowski oth Jan Skowron oth Krzysztof Ulaczyk oth Dorota Skowron oth Michal Pawlak oth Enthalten in Nature London : Macmillan Publishers Limited, part of Springer Nature, 1869 537(2016), 7622, Seite 649-651 (DE-627)129292834 (DE-600)120714-3 (DE-576)014473941 0028-0836 nnns volume:537 year:2016 number:7622 pages:649-651 http://dx.doi.org/10.1038/nature19066 Volltext http://search.proquest.com/docview/1825571603 http://arxiv.org/abs/1608.04753 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 537 2016 7622 649-651
spelling	10.1038/nature19066 doi PQ20170206 (DE-627)OLC1982122110 (DE-599)GBVOLC1982122110 (PRQ)a2081-a34e864c1852087018682baf039cdee6ef82fcaeccef5286a160f3f785cd077c0 (KEY)0072945020160000537762200649awakeningofaclassicalnovafromhibernation DE-627 ger DE-627 rakwb eng 070 500 DE-101 500 AVZ BIODIV fid Przemek Mróz verfasserin aut The awakening of a classical nova from hibernation 2016 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier Cataclysmic variable stars-novae, dwarf novae, and nova-likes-are close binary systems consisting of a white dwarf star (the primary) that is accreting matter from a low-mass companion star (the secondary)1. From time to time such systems undergo large-amplitude brightenings. The most spectacular eruptions, with a ten-thousandfold increase in brightness, occur in classical novae and are caused by a thermonuclear runaway on the surface of the white dwarf2. Such eruptions are thought to recur on timescales of ten thousand to a million years3. In between, the system's properties depend primarily on the mass-transfer rate: if it is lower than a billionth of a solar mass per year, the accretion becomes unstable and the matter is dumped onto the white dwarf during quasi-periodic dwarf nova outbursts4. The hibernation hypothesis5 predicts that nova eruptions strongly affect the mass-transfer rate in the binary, keeping it high for centuries after the event6. Subsequently, the mass-transfer rate should significantly decrease for a thousand to a million years, starting the hibernation phase. After that the nova awakes again-with accretion returning to the pre-eruption level and leading to a new nova explosion. The hibernation model predicts cyclical evolution of cataclysmic variables through phases of high and low mass-transfer. The theory gained some support from the discovery of ancient nova shells around the dwarf novae Z Camelopardalis7 and AT Cancri8, but direct evidence for considerable mass-transfer changes prior, during and after nova eruptions has not hitherto been found. Here we report long-term observations of the classical nova V1213 Cen (Nova Centauri 2009) covering its pre- and post-eruption phases and precisely documenting its evolution. Within the six years before the explosion, the system revealed dwarf nova outbursts indicative of a low mass-transfer rate. The post-nova is two orders of magnitude brighter than the pre-nova at minimum light with no trace of dwarf nova behaviour, implying that the mass-transfer rate increased considerably as a result of the nova explosion. White dwarfs Astronomy Accretion disks Observations Stars, New Solar and Stellar Astrophysics Astrophysics Andrzej Udalski oth Pawel Pietrukowicz oth Michal K Szymanski oth Igor Soszynski oth Lukasz Wyrzykowski oth Radoslaw Poleski oth Szymon Kozlowski oth Jan Skowron oth Krzysztof Ulaczyk oth Dorota Skowron oth Michal Pawlak oth Enthalten in Nature London : Macmillan Publishers Limited, part of Springer Nature, 1869 537(2016), 7622, Seite 649-651 (DE-627)129292834 (DE-600)120714-3 (DE-576)014473941 0028-0836 nnns volume:537 year:2016 number:7622 pages:649-651 http://dx.doi.org/10.1038/nature19066 Volltext http://search.proquest.com/docview/1825571603 http://arxiv.org/abs/1608.04753 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 537 2016 7622 649-651
allfields_unstemmed	10.1038/nature19066 doi PQ20170206 (DE-627)OLC1982122110 (DE-599)GBVOLC1982122110 (PRQ)a2081-a34e864c1852087018682baf039cdee6ef82fcaeccef5286a160f3f785cd077c0 (KEY)0072945020160000537762200649awakeningofaclassicalnovafromhibernation DE-627 ger DE-627 rakwb eng 070 500 DE-101 500 AVZ BIODIV fid Przemek Mróz verfasserin aut The awakening of a classical nova from hibernation 2016 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier Cataclysmic variable stars-novae, dwarf novae, and nova-likes-are close binary systems consisting of a white dwarf star (the primary) that is accreting matter from a low-mass companion star (the secondary)1. From time to time such systems undergo large-amplitude brightenings. The most spectacular eruptions, with a ten-thousandfold increase in brightness, occur in classical novae and are caused by a thermonuclear runaway on the surface of the white dwarf2. Such eruptions are thought to recur on timescales of ten thousand to a million years3. In between, the system's properties depend primarily on the mass-transfer rate: if it is lower than a billionth of a solar mass per year, the accretion becomes unstable and the matter is dumped onto the white dwarf during quasi-periodic dwarf nova outbursts4. The hibernation hypothesis5 predicts that nova eruptions strongly affect the mass-transfer rate in the binary, keeping it high for centuries after the event6. Subsequently, the mass-transfer rate should significantly decrease for a thousand to a million years, starting the hibernation phase. After that the nova awakes again-with accretion returning to the pre-eruption level and leading to a new nova explosion. The hibernation model predicts cyclical evolution of cataclysmic variables through phases of high and low mass-transfer. The theory gained some support from the discovery of ancient nova shells around the dwarf novae Z Camelopardalis7 and AT Cancri8, but direct evidence for considerable mass-transfer changes prior, during and after nova eruptions has not hitherto been found. Here we report long-term observations of the classical nova V1213 Cen (Nova Centauri 2009) covering its pre- and post-eruption phases and precisely documenting its evolution. Within the six years before the explosion, the system revealed dwarf nova outbursts indicative of a low mass-transfer rate. The post-nova is two orders of magnitude brighter than the pre-nova at minimum light with no trace of dwarf nova behaviour, implying that the mass-transfer rate increased considerably as a result of the nova explosion. White dwarfs Astronomy Accretion disks Observations Stars, New Solar and Stellar Astrophysics Astrophysics Andrzej Udalski oth Pawel Pietrukowicz oth Michal K Szymanski oth Igor Soszynski oth Lukasz Wyrzykowski oth Radoslaw Poleski oth Szymon Kozlowski oth Jan Skowron oth Krzysztof Ulaczyk oth Dorota Skowron oth Michal Pawlak oth Enthalten in Nature London : Macmillan Publishers Limited, part of Springer Nature, 1869 537(2016), 7622, Seite 649-651 (DE-627)129292834 (DE-600)120714-3 (DE-576)014473941 0028-0836 nnns volume:537 year:2016 number:7622 pages:649-651 http://dx.doi.org/10.1038/nature19066 Volltext http://search.proquest.com/docview/1825571603 http://arxiv.org/abs/1608.04753 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 537 2016 7622 649-651
allfieldsGer	10.1038/nature19066 doi PQ20170206 (DE-627)OLC1982122110 (DE-599)GBVOLC1982122110 (PRQ)a2081-a34e864c1852087018682baf039cdee6ef82fcaeccef5286a160f3f785cd077c0 (KEY)0072945020160000537762200649awakeningofaclassicalnovafromhibernation DE-627 ger DE-627 rakwb eng 070 500 DE-101 500 AVZ BIODIV fid Przemek Mróz verfasserin aut The awakening of a classical nova from hibernation 2016 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier Cataclysmic variable stars-novae, dwarf novae, and nova-likes-are close binary systems consisting of a white dwarf star (the primary) that is accreting matter from a low-mass companion star (the secondary)1. From time to time such systems undergo large-amplitude brightenings. The most spectacular eruptions, with a ten-thousandfold increase in brightness, occur in classical novae and are caused by a thermonuclear runaway on the surface of the white dwarf2. Such eruptions are thought to recur on timescales of ten thousand to a million years3. In between, the system's properties depend primarily on the mass-transfer rate: if it is lower than a billionth of a solar mass per year, the accretion becomes unstable and the matter is dumped onto the white dwarf during quasi-periodic dwarf nova outbursts4. The hibernation hypothesis5 predicts that nova eruptions strongly affect the mass-transfer rate in the binary, keeping it high for centuries after the event6. Subsequently, the mass-transfer rate should significantly decrease for a thousand to a million years, starting the hibernation phase. After that the nova awakes again-with accretion returning to the pre-eruption level and leading to a new nova explosion. The hibernation model predicts cyclical evolution of cataclysmic variables through phases of high and low mass-transfer. The theory gained some support from the discovery of ancient nova shells around the dwarf novae Z Camelopardalis7 and AT Cancri8, but direct evidence for considerable mass-transfer changes prior, during and after nova eruptions has not hitherto been found. Here we report long-term observations of the classical nova V1213 Cen (Nova Centauri 2009) covering its pre- and post-eruption phases and precisely documenting its evolution. Within the six years before the explosion, the system revealed dwarf nova outbursts indicative of a low mass-transfer rate. The post-nova is two orders of magnitude brighter than the pre-nova at minimum light with no trace of dwarf nova behaviour, implying that the mass-transfer rate increased considerably as a result of the nova explosion. White dwarfs Astronomy Accretion disks Observations Stars, New Solar and Stellar Astrophysics Astrophysics Andrzej Udalski oth Pawel Pietrukowicz oth Michal K Szymanski oth Igor Soszynski oth Lukasz Wyrzykowski oth Radoslaw Poleski oth Szymon Kozlowski oth Jan Skowron oth Krzysztof Ulaczyk oth Dorota Skowron oth Michal Pawlak oth Enthalten in Nature London : Macmillan Publishers Limited, part of Springer Nature, 1869 537(2016), 7622, Seite 649-651 (DE-627)129292834 (DE-600)120714-3 (DE-576)014473941 0028-0836 nnns volume:537 year:2016 number:7622 pages:649-651 http://dx.doi.org/10.1038/nature19066 Volltext http://search.proquest.com/docview/1825571603 http://arxiv.org/abs/1608.04753 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 537 2016 7622 649-651
allfieldsSound	10.1038/nature19066 doi PQ20170206 (DE-627)OLC1982122110 (DE-599)GBVOLC1982122110 (PRQ)a2081-a34e864c1852087018682baf039cdee6ef82fcaeccef5286a160f3f785cd077c0 (KEY)0072945020160000537762200649awakeningofaclassicalnovafromhibernation DE-627 ger DE-627 rakwb eng 070 500 DE-101 500 AVZ BIODIV fid Przemek Mróz verfasserin aut The awakening of a classical nova from hibernation 2016 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier Cataclysmic variable stars-novae, dwarf novae, and nova-likes-are close binary systems consisting of a white dwarf star (the primary) that is accreting matter from a low-mass companion star (the secondary)1. From time to time such systems undergo large-amplitude brightenings. The most spectacular eruptions, with a ten-thousandfold increase in brightness, occur in classical novae and are caused by a thermonuclear runaway on the surface of the white dwarf2. Such eruptions are thought to recur on timescales of ten thousand to a million years3. In between, the system's properties depend primarily on the mass-transfer rate: if it is lower than a billionth of a solar mass per year, the accretion becomes unstable and the matter is dumped onto the white dwarf during quasi-periodic dwarf nova outbursts4. The hibernation hypothesis5 predicts that nova eruptions strongly affect the mass-transfer rate in the binary, keeping it high for centuries after the event6. Subsequently, the mass-transfer rate should significantly decrease for a thousand to a million years, starting the hibernation phase. After that the nova awakes again-with accretion returning to the pre-eruption level and leading to a new nova explosion. The hibernation model predicts cyclical evolution of cataclysmic variables through phases of high and low mass-transfer. The theory gained some support from the discovery of ancient nova shells around the dwarf novae Z Camelopardalis7 and AT Cancri8, but direct evidence for considerable mass-transfer changes prior, during and after nova eruptions has not hitherto been found. Here we report long-term observations of the classical nova V1213 Cen (Nova Centauri 2009) covering its pre- and post-eruption phases and precisely documenting its evolution. Within the six years before the explosion, the system revealed dwarf nova outbursts indicative of a low mass-transfer rate. The post-nova is two orders of magnitude brighter than the pre-nova at minimum light with no trace of dwarf nova behaviour, implying that the mass-transfer rate increased considerably as a result of the nova explosion. White dwarfs Astronomy Accretion disks Observations Stars, New Solar and Stellar Astrophysics Astrophysics Andrzej Udalski oth Pawel Pietrukowicz oth Michal K Szymanski oth Igor Soszynski oth Lukasz Wyrzykowski oth Radoslaw Poleski oth Szymon Kozlowski oth Jan Skowron oth Krzysztof Ulaczyk oth Dorota Skowron oth Michal Pawlak oth Enthalten in Nature London : Macmillan Publishers Limited, part of Springer Nature, 1869 537(2016), 7622, Seite 649-651 (DE-627)129292834 (DE-600)120714-3 (DE-576)014473941 0028-0836 nnns volume:537 year:2016 number:7622 pages:649-651 http://dx.doi.org/10.1038/nature19066 Volltext http://search.proquest.com/docview/1825571603 http://arxiv.org/abs/1608.04753 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 537 2016 7622 649-651
language	English
source	Enthalten in Nature 537(2016), 7622, Seite 649-651 volume:537 year:2016 number:7622 pages:649-651
sourceStr	Enthalten in Nature 537(2016), 7622, Seite 649-651 volume:537 year:2016 number:7622 pages:649-651
format_phy_str_mv	Article
institution	findex.gbv.de
topic_facet	White dwarfs Astronomy Accretion disks Observations Stars, New Solar and Stellar Astrophysics Astrophysics
dewey-raw	070
isfreeaccess_bool	false
container_title	Nature
authorswithroles_txt_mv	Przemek Mróz @@aut@@ Andrzej Udalski @@oth@@ Pawel Pietrukowicz @@oth@@ Michal K Szymanski @@oth@@ Igor Soszynski @@oth@@ Lukasz Wyrzykowski @@oth@@ Radoslaw Poleski @@oth@@ Szymon Kozlowski @@oth@@ Jan Skowron @@oth@@ Krzysztof Ulaczyk @@oth@@ Dorota Skowron @@oth@@ Michal Pawlak @@oth@@
publishDateDaySort_date	2016-01-01T00:00:00Z
hierarchy_top_id	129292834
dewey-sort	270
id	OLC1982122110
language_de	englisch
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author	Przemek Mróz
spellingShingle	Przemek Mróz ddc 070 ddc 500 fid BIODIV misc White dwarfs misc Astronomy misc Accretion disks misc Observations misc Stars, New misc Solar and Stellar Astrophysics misc Astrophysics The awakening of a classical nova from hibernation
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title	The awakening of a classical nova from hibernation
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title_sort	awakening of a classical nova from hibernation
title_auth	The awakening of a classical nova from hibernation
abstract	Cataclysmic variable stars-novae, dwarf novae, and nova-likes-are close binary systems consisting of a white dwarf star (the primary) that is accreting matter from a low-mass companion star (the secondary)1. From time to time such systems undergo large-amplitude brightenings. The most spectacular eruptions, with a ten-thousandfold increase in brightness, occur in classical novae and are caused by a thermonuclear runaway on the surface of the white dwarf2. Such eruptions are thought to recur on timescales of ten thousand to a million years3. In between, the system's properties depend primarily on the mass-transfer rate: if it is lower than a billionth of a solar mass per year, the accretion becomes unstable and the matter is dumped onto the white dwarf during quasi-periodic dwarf nova outbursts4. The hibernation hypothesis5 predicts that nova eruptions strongly affect the mass-transfer rate in the binary, keeping it high for centuries after the event6. Subsequently, the mass-transfer rate should significantly decrease for a thousand to a million years, starting the hibernation phase. After that the nova awakes again-with accretion returning to the pre-eruption level and leading to a new nova explosion. The hibernation model predicts cyclical evolution of cataclysmic variables through phases of high and low mass-transfer. The theory gained some support from the discovery of ancient nova shells around the dwarf novae Z Camelopardalis7 and AT Cancri8, but direct evidence for considerable mass-transfer changes prior, during and after nova eruptions has not hitherto been found. Here we report long-term observations of the classical nova V1213 Cen (Nova Centauri 2009) covering its pre- and post-eruption phases and precisely documenting its evolution. Within the six years before the explosion, the system revealed dwarf nova outbursts indicative of a low mass-transfer rate. The post-nova is two orders of magnitude brighter than the pre-nova at minimum light with no trace of dwarf nova behaviour, implying that the mass-transfer rate increased considerably as a result of the nova explosion.
abstractGer	Cataclysmic variable stars-novae, dwarf novae, and nova-likes-are close binary systems consisting of a white dwarf star (the primary) that is accreting matter from a low-mass companion star (the secondary)1. From time to time such systems undergo large-amplitude brightenings. The most spectacular eruptions, with a ten-thousandfold increase in brightness, occur in classical novae and are caused by a thermonuclear runaway on the surface of the white dwarf2. Such eruptions are thought to recur on timescales of ten thousand to a million years3. In between, the system's properties depend primarily on the mass-transfer rate: if it is lower than a billionth of a solar mass per year, the accretion becomes unstable and the matter is dumped onto the white dwarf during quasi-periodic dwarf nova outbursts4. The hibernation hypothesis5 predicts that nova eruptions strongly affect the mass-transfer rate in the binary, keeping it high for centuries after the event6. Subsequently, the mass-transfer rate should significantly decrease for a thousand to a million years, starting the hibernation phase. After that the nova awakes again-with accretion returning to the pre-eruption level and leading to a new nova explosion. The hibernation model predicts cyclical evolution of cataclysmic variables through phases of high and low mass-transfer. The theory gained some support from the discovery of ancient nova shells around the dwarf novae Z Camelopardalis7 and AT Cancri8, but direct evidence for considerable mass-transfer changes prior, during and after nova eruptions has not hitherto been found. Here we report long-term observations of the classical nova V1213 Cen (Nova Centauri 2009) covering its pre- and post-eruption phases and precisely documenting its evolution. Within the six years before the explosion, the system revealed dwarf nova outbursts indicative of a low mass-transfer rate. The post-nova is two orders of magnitude brighter than the pre-nova at minimum light with no trace of dwarf nova behaviour, implying that the mass-transfer rate increased considerably as a result of the nova explosion.
abstract_unstemmed	Cataclysmic variable stars-novae, dwarf novae, and nova-likes-are close binary systems consisting of a white dwarf star (the primary) that is accreting matter from a low-mass companion star (the secondary)1. From time to time such systems undergo large-amplitude brightenings. The most spectacular eruptions, with a ten-thousandfold increase in brightness, occur in classical novae and are caused by a thermonuclear runaway on the surface of the white dwarf2. Such eruptions are thought to recur on timescales of ten thousand to a million years3. In between, the system's properties depend primarily on the mass-transfer rate: if it is lower than a billionth of a solar mass per year, the accretion becomes unstable and the matter is dumped onto the white dwarf during quasi-periodic dwarf nova outbursts4. The hibernation hypothesis5 predicts that nova eruptions strongly affect the mass-transfer rate in the binary, keeping it high for centuries after the event6. Subsequently, the mass-transfer rate should significantly decrease for a thousand to a million years, starting the hibernation phase. After that the nova awakes again-with accretion returning to the pre-eruption level and leading to a new nova explosion. The hibernation model predicts cyclical evolution of cataclysmic variables through phases of high and low mass-transfer. The theory gained some support from the discovery of ancient nova shells around the dwarf novae Z Camelopardalis7 and AT Cancri8, but direct evidence for considerable mass-transfer changes prior, during and after nova eruptions has not hitherto been found. Here we report long-term observations of the classical nova V1213 Cen (Nova Centauri 2009) covering its pre- and post-eruption phases and precisely documenting its evolution. Within the six years before the explosion, the system revealed dwarf nova outbursts indicative of a low mass-transfer rate. The post-nova is two orders of magnitude brighter than the pre-nova at minimum light with no trace of dwarf nova behaviour, implying that the mass-transfer rate increased considerably as a result of the nova explosion.
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container_issue	7622
title_short	The awakening of a classical nova from hibernation
url	http://dx.doi.org/10.1038/nature19066 http://search.proquest.com/docview/1825571603 http://arxiv.org/abs/1608.04753
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author2	Andrzej Udalski Pawel Pietrukowicz Michal K Szymanski Igor Soszynski Lukasz Wyrzykowski Radoslaw Poleski Szymon Kozlowski Jan Skowron Krzysztof Ulaczyk Dorota Skowron Michal Pawlak
author2Str	Andrzej Udalski Pawel Pietrukowicz Michal K Szymanski Igor Soszynski Lukasz Wyrzykowski Radoslaw Poleski Szymon Kozlowski Jan Skowron Krzysztof Ulaczyk Dorota Skowron Michal Pawlak
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From time to time such systems undergo large-amplitude brightenings. The most spectacular eruptions, with a ten-thousandfold increase in brightness, occur in classical novae and are caused by a thermonuclear runaway on the surface of the white dwarf2. Such eruptions are thought to recur on timescales of ten thousand to a million years3. In between, the system's properties depend primarily on the mass-transfer rate: if it is lower than a billionth of a solar mass per year, the accretion becomes unstable and the matter is dumped onto the white dwarf during quasi-periodic dwarf nova outbursts4. The hibernation hypothesis5 predicts that nova eruptions strongly affect the mass-transfer rate in the binary, keeping it high for centuries after the event6. Subsequently, the mass-transfer rate should significantly decrease for a thousand to a million years, starting the hibernation phase. After that the nova awakes again-with accretion returning to the pre-eruption level and leading to a new nova explosion. The hibernation model predicts cyclical evolution of cataclysmic variables through phases of high and low mass-transfer. The theory gained some support from the discovery of ancient nova shells around the dwarf novae Z Camelopardalis7 and AT Cancri8, but direct evidence for considerable mass-transfer changes prior, during and after nova eruptions has not hitherto been found. Here we report long-term observations of the classical nova V1213 Cen (Nova Centauri 2009) covering its pre- and post-eruption phases and precisely documenting its evolution. Within the six years before the explosion, the system revealed dwarf nova outbursts indicative of a low mass-transfer rate. The post-nova is two orders of magnitude brighter than the pre-nova at minimum light with no trace of dwarf nova behaviour, implying that the mass-transfer rate increased considerably as a result of the nova explosion.</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">White dwarfs</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Astronomy</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Accretion disks</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Observations</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Stars, New</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Solar and Stellar Astrophysics</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Astrophysics</subfield></datafield><datafield tag="700" ind1="0" ind2=" "><subfield code="a">Andrzej Udalski</subfield><subfield code="4">oth</subfield></datafield><datafield tag="700" ind1="0" ind2=" "><subfield code="a">Pawel Pietrukowicz</subfield><subfield code="4">oth</subfield></datafield><datafield tag="700" ind1="0" ind2=" "><subfield code="a">Michal K Szymanski</subfield><subfield code="4">oth</subfield></datafield><datafield tag="700" ind1="0" ind2=" "><subfield code="a">Igor Soszynski</subfield><subfield code="4">oth</subfield></datafield><datafield tag="700" ind1="0" ind2=" "><subfield code="a">Lukasz Wyrzykowski</subfield><subfield code="4">oth</subfield></datafield><datafield tag="700" ind1="0" ind2=" "><subfield code="a">Radoslaw Poleski</subfield><subfield code="4">oth</subfield></datafield><datafield tag="700" ind1="0" ind2=" "><subfield code="a">Szymon Kozlowski</subfield><subfield code="4">oth</subfield></datafield><datafield tag="700" ind1="0" ind2=" "><subfield code="a">Jan Skowron</subfield><subfield code="4">oth</subfield></datafield><datafield tag="700" 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The awakening of a classical nova from hibernation

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