Circumbinary Planetary Systems in the Solar Neighborhood: Stability and Habitability
Abstract The radii of the inner and outer boundaries of the circumbinary habitable zone (CBHZ) and the radii of the circumbinary chaotic zone (CBCZ) have been calculated for close binary stars in the solar neighborhood with sufficient catalogue data. A subclass of binaries for which the CBCZ boundar...
Ausführliche Beschreibung
Gespeichert in:
| Autor*in: |
Shevchenko, I. I. [verfasserIn] Melnikov, A. V. [verfasserIn] Popova, E. A. [verfasserIn] Bobylev, V. V. [verfasserIn] Karelin, G. M. [verfasserIn] |
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| Format: |
E-Artikel |
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| Sprache: |
Englisch |
| Erschienen: |
2019 |
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| Schlagwörter: |
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| Übergeordnetes Werk: |
Enthalten in: Astronomy letters - Moscow : MAIK Nauka/Interperiodika, 1993, 45(2019), 9 vom: Sept., Seite 620-626 |
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| Übergeordnetes Werk: |
volume:45 ; year:2019 ; number:9 ; month:09 ; pages:620-626 |
| Links: |
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| DOI / URN: |
10.1134/S1063773719080097 |
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| Katalog-ID: |
SPR019420862 |
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| 245 | 1 | 0 | |a Circumbinary Planetary Systems in the Solar Neighborhood: Stability and Habitability |
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| 520 | |a Abstract The radii of the inner and outer boundaries of the circumbinary habitable zone (CBHZ) and the radii of the circumbinary chaotic zone (CBCZ) have been calculated for close binary stars in the solar neighborhood with sufficient catalogue data. A subclass of binaries for which the CBCZ boundary is within the CBHZ boundaries (the CBCZ radius is larger than the inner CBHZ radius, but smaller than the outer CBHZ radius) has been identified for the first time: M4-V69, HATS551-027, EZ Aqr A–C, 38 Cas, HD 2070, HD 15064, HD 28394, HD 160346, and HD 181602. Since, according to present-day theories and observational data, the probability of finding planets at the CBCZ boundary is high, one might expect the presence of potentially habitable circumbinary planets in the planetary systems of the binary stars revealed in this way. For the stars CM Dra, WTS 19c-3-01405, and LP 661-13 the CBCZ radius is smaller than the radius of the inner CBHZ boundary, but planets may be present around them in outer stable orbits resonant with the orbits of planets near the CBCZ boundary. Therefore, all of the binaries of these types revealed for the first time are of considerable interest for future observations. | ||
| 650 | 4 | |a close binary stars |7 (dpeaa)DE-He213 | |
| 650 | 4 | |a solar neighborhood |7 (dpeaa)DE-He213 | |
| 650 | 4 | |a circumbinary planets |7 (dpeaa)DE-He213 | |
| 650 | 4 | |a habitability |7 (dpeaa)DE-He213 | |
| 650 | 4 | |a dynamical chaos |7 (dpeaa)DE-He213 | |
| 700 | 1 | |a Melnikov, A. V. |e verfasserin |4 aut | |
| 700 | 1 | |a Popova, E. A. |e verfasserin |4 aut | |
| 700 | 1 | |a Bobylev, V. V. |e verfasserin |4 aut | |
| 700 | 1 | |a Karelin, G. M. |e verfasserin |4 aut | |
| 773 | 0 | 8 | |i Enthalten in |t Astronomy letters |d Moscow : MAIK Nauka/Interperiodika, 1993 |g 45(2019), 9 vom: Sept., Seite 620-626 |w (DE-627)312181795 |w (DE-600)2010278-1 |x 1562-6873 |7 nnns |
| 773 | 1 | 8 | |g volume:45 |g year:2019 |g number:9 |g month:09 |g pages:620-626 |
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10.1134/S1063773719080097 doi (DE-627)SPR019420862 (SPR)S1063773719080097-e DE-627 ger DE-627 rakwb eng 520 ASE 39.00 bkl Shevchenko, I. I. verfasserin aut Circumbinary Planetary Systems in the Solar Neighborhood: Stability and Habitability 2019 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract The radii of the inner and outer boundaries of the circumbinary habitable zone (CBHZ) and the radii of the circumbinary chaotic zone (CBCZ) have been calculated for close binary stars in the solar neighborhood with sufficient catalogue data. A subclass of binaries for which the CBCZ boundary is within the CBHZ boundaries (the CBCZ radius is larger than the inner CBHZ radius, but smaller than the outer CBHZ radius) has been identified for the first time: M4-V69, HATS551-027, EZ Aqr A–C, 38 Cas, HD 2070, HD 15064, HD 28394, HD 160346, and HD 181602. Since, according to present-day theories and observational data, the probability of finding planets at the CBCZ boundary is high, one might expect the presence of potentially habitable circumbinary planets in the planetary systems of the binary stars revealed in this way. For the stars CM Dra, WTS 19c-3-01405, and LP 661-13 the CBCZ radius is smaller than the radius of the inner CBHZ boundary, but planets may be present around them in outer stable orbits resonant with the orbits of planets near the CBCZ boundary. Therefore, all of the binaries of these types revealed for the first time are of considerable interest for future observations. close binary stars (dpeaa)DE-He213 solar neighborhood (dpeaa)DE-He213 circumbinary planets (dpeaa)DE-He213 habitability (dpeaa)DE-He213 dynamical chaos (dpeaa)DE-He213 Melnikov, A. V. verfasserin aut Popova, E. A. verfasserin aut Bobylev, V. V. verfasserin aut Karelin, G. M. verfasserin aut Enthalten in Astronomy letters Moscow : MAIK Nauka/Interperiodika, 1993 45(2019), 9 vom: Sept., Seite 620-626 (DE-627)312181795 (DE-600)2010278-1 1562-6873 nnns volume:45 year:2019 number:9 month:09 pages:620-626 https://dx.doi.org/10.1134/S1063773719080097 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER SSG-OPC-AST SSG-OPC-ASE GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_138 GBV_ILN_150 GBV_ILN_151 GBV_ILN_152 GBV_ILN_161 GBV_ILN_170 GBV_ILN_171 GBV_ILN_187 GBV_ILN_206 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_636 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2056 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_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 39.00 ASE AR 45 2019 9 09 620-626 |
| spelling |
10.1134/S1063773719080097 doi (DE-627)SPR019420862 (SPR)S1063773719080097-e DE-627 ger DE-627 rakwb eng 520 ASE 39.00 bkl Shevchenko, I. I. verfasserin aut Circumbinary Planetary Systems in the Solar Neighborhood: Stability and Habitability 2019 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract The radii of the inner and outer boundaries of the circumbinary habitable zone (CBHZ) and the radii of the circumbinary chaotic zone (CBCZ) have been calculated for close binary stars in the solar neighborhood with sufficient catalogue data. A subclass of binaries for which the CBCZ boundary is within the CBHZ boundaries (the CBCZ radius is larger than the inner CBHZ radius, but smaller than the outer CBHZ radius) has been identified for the first time: M4-V69, HATS551-027, EZ Aqr A–C, 38 Cas, HD 2070, HD 15064, HD 28394, HD 160346, and HD 181602. Since, according to present-day theories and observational data, the probability of finding planets at the CBCZ boundary is high, one might expect the presence of potentially habitable circumbinary planets in the planetary systems of the binary stars revealed in this way. For the stars CM Dra, WTS 19c-3-01405, and LP 661-13 the CBCZ radius is smaller than the radius of the inner CBHZ boundary, but planets may be present around them in outer stable orbits resonant with the orbits of planets near the CBCZ boundary. Therefore, all of the binaries of these types revealed for the first time are of considerable interest for future observations. close binary stars (dpeaa)DE-He213 solar neighborhood (dpeaa)DE-He213 circumbinary planets (dpeaa)DE-He213 habitability (dpeaa)DE-He213 dynamical chaos (dpeaa)DE-He213 Melnikov, A. V. verfasserin aut Popova, E. A. verfasserin aut Bobylev, V. V. verfasserin aut Karelin, G. M. verfasserin aut Enthalten in Astronomy letters Moscow : MAIK Nauka/Interperiodika, 1993 45(2019), 9 vom: Sept., Seite 620-626 (DE-627)312181795 (DE-600)2010278-1 1562-6873 nnns volume:45 year:2019 number:9 month:09 pages:620-626 https://dx.doi.org/10.1134/S1063773719080097 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER SSG-OPC-AST SSG-OPC-ASE GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_138 GBV_ILN_150 GBV_ILN_151 GBV_ILN_152 GBV_ILN_161 GBV_ILN_170 GBV_ILN_171 GBV_ILN_187 GBV_ILN_206 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_636 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2056 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_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 39.00 ASE AR 45 2019 9 09 620-626 |
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10.1134/S1063773719080097 doi (DE-627)SPR019420862 (SPR)S1063773719080097-e DE-627 ger DE-627 rakwb eng 520 ASE 39.00 bkl Shevchenko, I. I. verfasserin aut Circumbinary Planetary Systems in the Solar Neighborhood: Stability and Habitability 2019 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract The radii of the inner and outer boundaries of the circumbinary habitable zone (CBHZ) and the radii of the circumbinary chaotic zone (CBCZ) have been calculated for close binary stars in the solar neighborhood with sufficient catalogue data. A subclass of binaries for which the CBCZ boundary is within the CBHZ boundaries (the CBCZ radius is larger than the inner CBHZ radius, but smaller than the outer CBHZ radius) has been identified for the first time: M4-V69, HATS551-027, EZ Aqr A–C, 38 Cas, HD 2070, HD 15064, HD 28394, HD 160346, and HD 181602. Since, according to present-day theories and observational data, the probability of finding planets at the CBCZ boundary is high, one might expect the presence of potentially habitable circumbinary planets in the planetary systems of the binary stars revealed in this way. For the stars CM Dra, WTS 19c-3-01405, and LP 661-13 the CBCZ radius is smaller than the radius of the inner CBHZ boundary, but planets may be present around them in outer stable orbits resonant with the orbits of planets near the CBCZ boundary. Therefore, all of the binaries of these types revealed for the first time are of considerable interest for future observations. close binary stars (dpeaa)DE-He213 solar neighborhood (dpeaa)DE-He213 circumbinary planets (dpeaa)DE-He213 habitability (dpeaa)DE-He213 dynamical chaos (dpeaa)DE-He213 Melnikov, A. V. verfasserin aut Popova, E. A. verfasserin aut Bobylev, V. V. verfasserin aut Karelin, G. M. verfasserin aut Enthalten in Astronomy letters Moscow : MAIK Nauka/Interperiodika, 1993 45(2019), 9 vom: Sept., Seite 620-626 (DE-627)312181795 (DE-600)2010278-1 1562-6873 nnns volume:45 year:2019 number:9 month:09 pages:620-626 https://dx.doi.org/10.1134/S1063773719080097 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER SSG-OPC-AST SSG-OPC-ASE GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_138 GBV_ILN_150 GBV_ILN_151 GBV_ILN_152 GBV_ILN_161 GBV_ILN_170 GBV_ILN_171 GBV_ILN_187 GBV_ILN_206 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_636 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2056 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_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 39.00 ASE AR 45 2019 9 09 620-626 |
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10.1134/S1063773719080097 doi (DE-627)SPR019420862 (SPR)S1063773719080097-e DE-627 ger DE-627 rakwb eng 520 ASE 39.00 bkl Shevchenko, I. I. verfasserin aut Circumbinary Planetary Systems in the Solar Neighborhood: Stability and Habitability 2019 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract The radii of the inner and outer boundaries of the circumbinary habitable zone (CBHZ) and the radii of the circumbinary chaotic zone (CBCZ) have been calculated for close binary stars in the solar neighborhood with sufficient catalogue data. A subclass of binaries for which the CBCZ boundary is within the CBHZ boundaries (the CBCZ radius is larger than the inner CBHZ radius, but smaller than the outer CBHZ radius) has been identified for the first time: M4-V69, HATS551-027, EZ Aqr A–C, 38 Cas, HD 2070, HD 15064, HD 28394, HD 160346, and HD 181602. Since, according to present-day theories and observational data, the probability of finding planets at the CBCZ boundary is high, one might expect the presence of potentially habitable circumbinary planets in the planetary systems of the binary stars revealed in this way. For the stars CM Dra, WTS 19c-3-01405, and LP 661-13 the CBCZ radius is smaller than the radius of the inner CBHZ boundary, but planets may be present around them in outer stable orbits resonant with the orbits of planets near the CBCZ boundary. Therefore, all of the binaries of these types revealed for the first time are of considerable interest for future observations. close binary stars (dpeaa)DE-He213 solar neighborhood (dpeaa)DE-He213 circumbinary planets (dpeaa)DE-He213 habitability (dpeaa)DE-He213 dynamical chaos (dpeaa)DE-He213 Melnikov, A. V. verfasserin aut Popova, E. A. verfasserin aut Bobylev, V. V. verfasserin aut Karelin, G. M. verfasserin aut Enthalten in Astronomy letters Moscow : MAIK Nauka/Interperiodika, 1993 45(2019), 9 vom: Sept., Seite 620-626 (DE-627)312181795 (DE-600)2010278-1 1562-6873 nnns volume:45 year:2019 number:9 month:09 pages:620-626 https://dx.doi.org/10.1134/S1063773719080097 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER SSG-OPC-AST SSG-OPC-ASE GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_138 GBV_ILN_150 GBV_ILN_151 GBV_ILN_152 GBV_ILN_161 GBV_ILN_170 GBV_ILN_171 GBV_ILN_187 GBV_ILN_206 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_636 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2056 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_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 39.00 ASE AR 45 2019 9 09 620-626 |
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10.1134/S1063773719080097 doi (DE-627)SPR019420862 (SPR)S1063773719080097-e DE-627 ger DE-627 rakwb eng 520 ASE 39.00 bkl Shevchenko, I. I. verfasserin aut Circumbinary Planetary Systems in the Solar Neighborhood: Stability and Habitability 2019 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract The radii of the inner and outer boundaries of the circumbinary habitable zone (CBHZ) and the radii of the circumbinary chaotic zone (CBCZ) have been calculated for close binary stars in the solar neighborhood with sufficient catalogue data. A subclass of binaries for which the CBCZ boundary is within the CBHZ boundaries (the CBCZ radius is larger than the inner CBHZ radius, but smaller than the outer CBHZ radius) has been identified for the first time: M4-V69, HATS551-027, EZ Aqr A–C, 38 Cas, HD 2070, HD 15064, HD 28394, HD 160346, and HD 181602. Since, according to present-day theories and observational data, the probability of finding planets at the CBCZ boundary is high, one might expect the presence of potentially habitable circumbinary planets in the planetary systems of the binary stars revealed in this way. For the stars CM Dra, WTS 19c-3-01405, and LP 661-13 the CBCZ radius is smaller than the radius of the inner CBHZ boundary, but planets may be present around them in outer stable orbits resonant with the orbits of planets near the CBCZ boundary. Therefore, all of the binaries of these types revealed for the first time are of considerable interest for future observations. close binary stars (dpeaa)DE-He213 solar neighborhood (dpeaa)DE-He213 circumbinary planets (dpeaa)DE-He213 habitability (dpeaa)DE-He213 dynamical chaos (dpeaa)DE-He213 Melnikov, A. V. verfasserin aut Popova, E. A. verfasserin aut Bobylev, V. V. verfasserin aut Karelin, G. M. verfasserin aut Enthalten in Astronomy letters Moscow : MAIK Nauka/Interperiodika, 1993 45(2019), 9 vom: Sept., Seite 620-626 (DE-627)312181795 (DE-600)2010278-1 1562-6873 nnns volume:45 year:2019 number:9 month:09 pages:620-626 https://dx.doi.org/10.1134/S1063773719080097 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER SSG-OPC-AST SSG-OPC-ASE GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_138 GBV_ILN_150 GBV_ILN_151 GBV_ILN_152 GBV_ILN_161 GBV_ILN_170 GBV_ILN_171 GBV_ILN_187 GBV_ILN_206 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_636 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2056 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_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 39.00 ASE AR 45 2019 9 09 620-626 |
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Shevchenko, I. I. @@aut@@ Melnikov, A. V. @@aut@@ Popova, E. A. @@aut@@ Bobylev, V. V. @@aut@@ Karelin, G. M. @@aut@@ |
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I.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="245" ind1="1" ind2="0"><subfield code="a">Circumbinary Planetary Systems in the Solar Neighborhood: Stability and Habitability</subfield></datafield><datafield tag="264" ind1=" " ind2="1"><subfield code="c">2019</subfield></datafield><datafield tag="336" ind1=" " ind2=" "><subfield code="a">Text</subfield><subfield code="b">txt</subfield><subfield code="2">rdacontent</subfield></datafield><datafield tag="337" ind1=" " ind2=" "><subfield code="a">Computermedien</subfield><subfield code="b">c</subfield><subfield code="2">rdamedia</subfield></datafield><datafield tag="338" ind1=" " ind2=" "><subfield code="a">Online-Ressource</subfield><subfield code="b">cr</subfield><subfield code="2">rdacarrier</subfield></datafield><datafield tag="520" ind1=" " ind2=" "><subfield code="a">Abstract The radii of the inner and outer boundaries of the circumbinary habitable zone (CBHZ) and the radii of the circumbinary chaotic zone (CBCZ) have been calculated for close binary stars in the solar neighborhood with sufficient catalogue data. A subclass of binaries for which the CBCZ boundary is within the CBHZ boundaries (the CBCZ radius is larger than the inner CBHZ radius, but smaller than the outer CBHZ radius) has been identified for the first time: M4-V69, HATS551-027, EZ Aqr A–C, 38 Cas, HD 2070, HD 15064, HD 28394, HD 160346, and HD 181602. Since, according to present-day theories and observational data, the probability of finding planets at the CBCZ boundary is high, one might expect the presence of potentially habitable circumbinary planets in the planetary systems of the binary stars revealed in this way. For the stars CM Dra, WTS 19c-3-01405, and LP 661-13 the CBCZ radius is smaller than the radius of the inner CBHZ boundary, but planets may be present around them in outer stable orbits resonant with the orbits of planets near the CBCZ boundary. 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Shevchenko, I. I. |
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Shevchenko, I. I. ddc 520 bkl 39.00 misc close binary stars misc solar neighborhood misc circumbinary planets misc habitability misc dynamical chaos Circumbinary Planetary Systems in the Solar Neighborhood: Stability and Habitability |
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520 ASE 39.00 bkl Circumbinary Planetary Systems in the Solar Neighborhood: Stability and Habitability close binary stars (dpeaa)DE-He213 solar neighborhood (dpeaa)DE-He213 circumbinary planets (dpeaa)DE-He213 habitability (dpeaa)DE-He213 dynamical chaos (dpeaa)DE-He213 |
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ddc 520 bkl 39.00 misc close binary stars misc solar neighborhood misc circumbinary planets misc habitability misc dynamical chaos |
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Circumbinary Planetary Systems in the Solar Neighborhood: Stability and Habitability |
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Circumbinary Planetary Systems in the Solar Neighborhood: Stability and Habitability |
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circumbinary planetary systems in the solar neighborhood: stability and habitability |
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Circumbinary Planetary Systems in the Solar Neighborhood: Stability and Habitability |
| abstract |
Abstract The radii of the inner and outer boundaries of the circumbinary habitable zone (CBHZ) and the radii of the circumbinary chaotic zone (CBCZ) have been calculated for close binary stars in the solar neighborhood with sufficient catalogue data. A subclass of binaries for which the CBCZ boundary is within the CBHZ boundaries (the CBCZ radius is larger than the inner CBHZ radius, but smaller than the outer CBHZ radius) has been identified for the first time: M4-V69, HATS551-027, EZ Aqr A–C, 38 Cas, HD 2070, HD 15064, HD 28394, HD 160346, and HD 181602. Since, according to present-day theories and observational data, the probability of finding planets at the CBCZ boundary is high, one might expect the presence of potentially habitable circumbinary planets in the planetary systems of the binary stars revealed in this way. For the stars CM Dra, WTS 19c-3-01405, and LP 661-13 the CBCZ radius is smaller than the radius of the inner CBHZ boundary, but planets may be present around them in outer stable orbits resonant with the orbits of planets near the CBCZ boundary. Therefore, all of the binaries of these types revealed for the first time are of considerable interest for future observations. |
| abstractGer |
Abstract The radii of the inner and outer boundaries of the circumbinary habitable zone (CBHZ) and the radii of the circumbinary chaotic zone (CBCZ) have been calculated for close binary stars in the solar neighborhood with sufficient catalogue data. A subclass of binaries for which the CBCZ boundary is within the CBHZ boundaries (the CBCZ radius is larger than the inner CBHZ radius, but smaller than the outer CBHZ radius) has been identified for the first time: M4-V69, HATS551-027, EZ Aqr A–C, 38 Cas, HD 2070, HD 15064, HD 28394, HD 160346, and HD 181602. Since, according to present-day theories and observational data, the probability of finding planets at the CBCZ boundary is high, one might expect the presence of potentially habitable circumbinary planets in the planetary systems of the binary stars revealed in this way. For the stars CM Dra, WTS 19c-3-01405, and LP 661-13 the CBCZ radius is smaller than the radius of the inner CBHZ boundary, but planets may be present around them in outer stable orbits resonant with the orbits of planets near the CBCZ boundary. Therefore, all of the binaries of these types revealed for the first time are of considerable interest for future observations. |
| abstract_unstemmed |
Abstract The radii of the inner and outer boundaries of the circumbinary habitable zone (CBHZ) and the radii of the circumbinary chaotic zone (CBCZ) have been calculated for close binary stars in the solar neighborhood with sufficient catalogue data. A subclass of binaries for which the CBCZ boundary is within the CBHZ boundaries (the CBCZ radius is larger than the inner CBHZ radius, but smaller than the outer CBHZ radius) has been identified for the first time: M4-V69, HATS551-027, EZ Aqr A–C, 38 Cas, HD 2070, HD 15064, HD 28394, HD 160346, and HD 181602. Since, according to present-day theories and observational data, the probability of finding planets at the CBCZ boundary is high, one might expect the presence of potentially habitable circumbinary planets in the planetary systems of the binary stars revealed in this way. For the stars CM Dra, WTS 19c-3-01405, and LP 661-13 the CBCZ radius is smaller than the radius of the inner CBHZ boundary, but planets may be present around them in outer stable orbits resonant with the orbits of planets near the CBCZ boundary. Therefore, all of the binaries of these types revealed for the first time are of considerable interest for future observations. |
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9 |
| title_short |
Circumbinary Planetary Systems in the Solar Neighborhood: Stability and Habitability |
| url |
https://dx.doi.org/10.1134/S1063773719080097 |
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| author2 |
Melnikov, A. V. Popova, E. A. Bobylev, V. V. Karelin, G. M. |
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Melnikov, A. V. Popova, E. A. Bobylev, V. V. Karelin, G. M. |
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| doi_str |
10.1134/S1063773719080097 |
| up_date |
2024-07-04T01:32:13.746Z |
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| score |
7.4003057 |