Interacting winds in classical nova outbursts
| ISSN: |
1572-946X
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|---|---|
| Keywords: |
Novae ; Numerical Hydrodynamics
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| Source: |
Springer Online Journal Archives 1860-2000
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| Topics: |
Physics
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| Notes: |
Abstract Classical nova outbursts occur in binary systems containing a white dwarf accretor and a Roche-lobe-filling main-sequence star. The outburst is due to a thermonuclear runaway in the accreted material on the surface of the white dwarf, and results in the ejection of up to 10−4 M ⊙of material at velocities of several hundred to a few thousand kilometres per second. There is now strong evidence that the mass ejection takes place via a wind with secularly increasing velocity. The fast ejecta catches up with slower moving material ejected earlier in the outburst, forming a layer of shock-heated gas which gives rise to a short burst of soft X-ray emission. This emission was observed in V838 Her (Nova Herculis 1991), and was succesfully accounted for by the ‘interacting winds’ model. In this paper, we present 2.5-D numerical hydrodynamics calculations of interacting winds in novae which consider the effects of the binary system on shaping the mass-loss, and show that many of the features seen in the optical shells of novae many years after outburst can be accounted for.
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| Type of Medium: |
Electronic Resource
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| URL: |
| _version_ | 1798296450518482944 |
|---|---|
| autor | Lloyd, H. M. O'Brien, T. J. Bode, M. F. |
| autorsonst | Lloyd, H. M. O'Brien, T. J. Bode, M. F. |
| book_url | http://dx.doi.org/10.1007/BF00627366 |
| datenlieferant | nat_lic_papers |
| hauptsatz | hsatz_simple |
| identnr | NLM193065746 |
| issn | 1572-946X |
| journal_name | Astrophysics and space science |
| materialart | 1 |
| notes | Abstract Classical nova outbursts occur in binary systems containing a white dwarf accretor and a Roche-lobe-filling main-sequence star. The outburst is due to a thermonuclear runaway in the accreted material on the surface of the white dwarf, and results in the ejection of up to 10−4 M ⊙of material at velocities of several hundred to a few thousand kilometres per second. There is now strong evidence that the mass ejection takes place via a wind with secularly increasing velocity. The fast ejecta catches up with slower moving material ejected earlier in the outburst, forming a layer of shock-heated gas which gives rise to a short burst of soft X-ray emission. This emission was observed in V838 Her (Nova Herculis 1991), and was succesfully accounted for by the ‘interacting winds’ model. In this paper, we present 2.5-D numerical hydrodynamics calculations of interacting winds in novae which consider the effects of the binary system on shaping the mass-loss, and show that many of the features seen in the optical shells of novae many years after outburst can be accounted for. |
| package_name | Springer |
| publikationsjahr_anzeige | 1995 |
| publikationsjahr_facette | 1995 |
| publikationsjahr_intervall | 8004:1995-1999 |
| publikationsjahr_sort | 1995 |
| publisher | Springer |
| reference | 233 (1995), S. 317-321 |
| schlagwort | Novae Numerical Hydrodynamics |
| search_space | articles |
| shingle_author_1 | Lloyd, H. M. O'Brien, T. J. Bode, M. F. |
| shingle_author_2 | Lloyd, H. M. O'Brien, T. J. Bode, M. F. |
| shingle_author_3 | Lloyd, H. M. O'Brien, T. J. Bode, M. F. |
| shingle_author_4 | Lloyd, H. M. O'Brien, T. J. Bode, M. F. |
| shingle_catch_all_1 | Lloyd, H. M. O'Brien, T. J. Bode, M. F. Interacting winds in classical nova outbursts Novae Numerical Hydrodynamics Novae Numerical Hydrodynamics Abstract Classical nova outbursts occur in binary systems containing a white dwarf accretor and a Roche-lobe-filling main-sequence star. The outburst is due to a thermonuclear runaway in the accreted material on the surface of the white dwarf, and results in the ejection of up to 10−4 M ⊙of material at velocities of several hundred to a few thousand kilometres per second. There is now strong evidence that the mass ejection takes place via a wind with secularly increasing velocity. The fast ejecta catches up with slower moving material ejected earlier in the outburst, forming a layer of shock-heated gas which gives rise to a short burst of soft X-ray emission. This emission was observed in V838 Her (Nova Herculis 1991), and was succesfully accounted for by the ‘interacting winds’ model. In this paper, we present 2.5-D numerical hydrodynamics calculations of interacting winds in novae which consider the effects of the binary system on shaping the mass-loss, and show that many of the features seen in the optical shells of novae many years after outburst can be accounted for. 1572-946X 1572946X Springer |
| shingle_catch_all_2 | Lloyd, H. M. O'Brien, T. J. Bode, M. F. Interacting winds in classical nova outbursts Novae Numerical Hydrodynamics Novae Numerical Hydrodynamics Abstract Classical nova outbursts occur in binary systems containing a white dwarf accretor and a Roche-lobe-filling main-sequence star. The outburst is due to a thermonuclear runaway in the accreted material on the surface of the white dwarf, and results in the ejection of up to 10−4 M ⊙of material at velocities of several hundred to a few thousand kilometres per second. There is now strong evidence that the mass ejection takes place via a wind with secularly increasing velocity. The fast ejecta catches up with slower moving material ejected earlier in the outburst, forming a layer of shock-heated gas which gives rise to a short burst of soft X-ray emission. This emission was observed in V838 Her (Nova Herculis 1991), and was succesfully accounted for by the ‘interacting winds’ model. In this paper, we present 2.5-D numerical hydrodynamics calculations of interacting winds in novae which consider the effects of the binary system on shaping the mass-loss, and show that many of the features seen in the optical shells of novae many years after outburst can be accounted for. 1572-946X 1572946X Springer |
| shingle_catch_all_3 | Lloyd, H. M. O'Brien, T. J. Bode, M. F. Interacting winds in classical nova outbursts Novae Numerical Hydrodynamics Novae Numerical Hydrodynamics Abstract Classical nova outbursts occur in binary systems containing a white dwarf accretor and a Roche-lobe-filling main-sequence star. The outburst is due to a thermonuclear runaway in the accreted material on the surface of the white dwarf, and results in the ejection of up to 10−4 M ⊙of material at velocities of several hundred to a few thousand kilometres per second. There is now strong evidence that the mass ejection takes place via a wind with secularly increasing velocity. The fast ejecta catches up with slower moving material ejected earlier in the outburst, forming a layer of shock-heated gas which gives rise to a short burst of soft X-ray emission. This emission was observed in V838 Her (Nova Herculis 1991), and was succesfully accounted for by the ‘interacting winds’ model. In this paper, we present 2.5-D numerical hydrodynamics calculations of interacting winds in novae which consider the effects of the binary system on shaping the mass-loss, and show that many of the features seen in the optical shells of novae many years after outburst can be accounted for. 1572-946X 1572946X Springer |
| shingle_catch_all_4 | Lloyd, H. M. O'Brien, T. J. Bode, M. F. Interacting winds in classical nova outbursts Novae Numerical Hydrodynamics Novae Numerical Hydrodynamics Abstract Classical nova outbursts occur in binary systems containing a white dwarf accretor and a Roche-lobe-filling main-sequence star. The outburst is due to a thermonuclear runaway in the accreted material on the surface of the white dwarf, and results in the ejection of up to 10−4 M ⊙of material at velocities of several hundred to a few thousand kilometres per second. There is now strong evidence that the mass ejection takes place via a wind with secularly increasing velocity. The fast ejecta catches up with slower moving material ejected earlier in the outburst, forming a layer of shock-heated gas which gives rise to a short burst of soft X-ray emission. This emission was observed in V838 Her (Nova Herculis 1991), and was succesfully accounted for by the ‘interacting winds’ model. In this paper, we present 2.5-D numerical hydrodynamics calculations of interacting winds in novae which consider the effects of the binary system on shaping the mass-loss, and show that many of the features seen in the optical shells of novae many years after outburst can be accounted for. 1572-946X 1572946X Springer |
| shingle_title_1 | Interacting winds in classical nova outbursts |
| shingle_title_2 | Interacting winds in classical nova outbursts |
| shingle_title_3 | Interacting winds in classical nova outbursts |
| shingle_title_4 | Interacting winds in classical nova outbursts |
| sigel_instance_filter | dkfz geomar wilbert ipn albert fhp |
| source_archive | Springer Online Journal Archives 1860-2000 |
| timestamp | 2024-05-06T09:52:17.473Z |
| titel | Interacting winds in classical nova outbursts |
| titel_suche | Interacting winds in classical nova outbursts |
| topic | U |
| uid | nat_lic_papers_NLM193065746 |