DOUBLE BOW SHOCKS AROUND YOUNG, RUNAWAY RED SUPERGIANTS: APPLICATION TO BETELGEUSE
A significant fraction of massive stars are moving supersonically through the interstellar medium (ISM), either due to disruption of a binary system or ejection from their parent star cluster. The interaction of their wind with the ISM produces a bow shock. In late evolutionary stages these stars ma...
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| Veröffentlicht in: | Astrophysical journal. Letters 2012-05, Vol.751 (1), p.1-6 |
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| creator | Mackey, Jonathan MOHAMED, SHAZRENE NEILSON, HILDING R Langer, Norbert Meyer, M-A |
| description | A significant fraction of massive stars are moving supersonically through the interstellar medium (ISM), either due to disruption of a binary system or ejection from their parent star cluster. The interaction of their wind with the ISM produces a bow shock. In late evolutionary stages these stars may undergo rapid transitions from red to blue and vice versa on the Hertzsprung-Russell diagram, with accompanying rapid changes to their stellar winds and bow shocks. Recent three-dimensional simulations of the bow shock produced by the nearby runaway red supergiant (RSG) Betelgeuse, under the assumption of a constant wind, indicate that the bow shock is very young ( |
| doi_str_mv | 10.1088/2041-8205/751/1/L10 |
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The interaction of their wind with the ISM produces a bow shock. In late evolutionary stages these stars may undergo rapid transitions from red to blue and vice versa on the Hertzsprung-Russell diagram, with accompanying rapid changes to their stellar winds and bow shocks. Recent three-dimensional simulations of the bow shock produced by the nearby runaway red supergiant (RSG) Betelgeuse, under the assumption of a constant wind, indicate that the bow shock is very young (<30,000 years old), hence Betelgeuse may have only recently become an RSG. To test this possibility, we have calculated stellar evolution models for single stars which match the observed properties of Betelgeuse in the RSG phase. The resulting evolving stellar wind is incorporated into two-dimensional hydrodynamic simulations in which we model a runaway blue supergiant (BSG) as it undergoes the transition to an RSG near the end of its life. We find that the collapsing BSG wind bubble induces a bow shock-shaped inner shell around the RSG wind that resembles Betelgeuse's bow shock, and has a similar mass. Surrounding this is the larger-scale retreating bow shock generated by the now defunct BSG wind's interaction with the ISM. We suggest that this outer shell could explain the bar feature located (at least in projection) just in front of Betelgeuse's bow shock.</description><identifier>ISSN: 2041-8205</identifier><identifier>EISSN: 2041-8213</identifier><identifier>DOI: 10.1088/2041-8205/751/1/L10</identifier><language>eng</language><publisher>United States</publisher><subject>Astronomical models ; ASTROPHYSICS ; ASTROPHYSICS, COSMOLOGY AND ASTRONOMY ; BINARY STARS ; Computer simulation ; Constants ; Evolutionary ; HERTZSPRUNG-RUSSELL DIAGRAM ; HYDRODYNAMICS ; INTERSTELLAR SPACE ; MASS ; RED GIANT STARS ; Shells ; SHOCK WAVES ; STAR CLUSTERS ; STAR EVOLUTION ; Stars ; STELLAR WINDS ; Three dimensional ; THREE-DIMENSIONAL CALCULATIONS ; TWO-DIMENSIONAL CALCULATIONS</subject><ispartof>Astrophysical journal. 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Letters</title><description>A significant fraction of massive stars are moving supersonically through the interstellar medium (ISM), either due to disruption of a binary system or ejection from their parent star cluster. The interaction of their wind with the ISM produces a bow shock. In late evolutionary stages these stars may undergo rapid transitions from red to blue and vice versa on the Hertzsprung-Russell diagram, with accompanying rapid changes to their stellar winds and bow shocks. Recent three-dimensional simulations of the bow shock produced by the nearby runaway red supergiant (RSG) Betelgeuse, under the assumption of a constant wind, indicate that the bow shock is very young (<30,000 years old), hence Betelgeuse may have only recently become an RSG. To test this possibility, we have calculated stellar evolution models for single stars which match the observed properties of Betelgeuse in the RSG phase. The resulting evolving stellar wind is incorporated into two-dimensional hydrodynamic simulations in which we model a runaway blue supergiant (BSG) as it undergoes the transition to an RSG near the end of its life. We find that the collapsing BSG wind bubble induces a bow shock-shaped inner shell around the RSG wind that resembles Betelgeuse's bow shock, and has a similar mass. Surrounding this is the larger-scale retreating bow shock generated by the now defunct BSG wind's interaction with the ISM. We suggest that this outer shell could explain the bar feature located (at least in projection) just in front of Betelgeuse's bow shock.</description><subject>Astronomical models</subject><subject>ASTROPHYSICS</subject><subject>ASTROPHYSICS, COSMOLOGY AND ASTRONOMY</subject><subject>BINARY STARS</subject><subject>Computer simulation</subject><subject>Constants</subject><subject>Evolutionary</subject><subject>HERTZSPRUNG-RUSSELL DIAGRAM</subject><subject>HYDRODYNAMICS</subject><subject>INTERSTELLAR SPACE</subject><subject>MASS</subject><subject>RED GIANT STARS</subject><subject>Shells</subject><subject>SHOCK WAVES</subject><subject>STAR CLUSTERS</subject><subject>STAR EVOLUTION</subject><subject>Stars</subject><subject>STELLAR WINDS</subject><subject>Three dimensional</subject><subject>THREE-DIMENSIONAL CALCULATIONS</subject><subject>TWO-DIMENSIONAL CALCULATIONS</subject><issn>2041-8205</issn><issn>2041-8213</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2012</creationdate><recordtype>article</recordtype><recordid>eNqNj01Lw0AURQdRsFZ_gZsBNy6Mme-ZuEvbMS2GTMkHpauQTqZYqY066f830OLazbuHy3kPHgD3GD1jpFRIEMOBIoiHkuMQhylGF2B0bjG9_GPEr8GN9x8IESSwGoF8ZqpJquHErGAxN9O3Asa5qbIZXA8zeYJ5lcWreA1zPYNFtdR5soizsniB8XKZLqZxuTAZLA2c6FKnia4KfQuuts3eu7tzjkH5qsvpPEhNMiykQUdY1AcsckhJ6ZzijcItk4K31LYbQbh0G0SJ5O1GCsoHFC2nkgnXNBbxiKhtQ-kYPJzOdr7f1d7uemffbXc4ONvXZPhXKiwG6_Fkff1030fn-_pz563b75uD646-xkJEEWZIkf-oDEeYEE5_AfMuZOE</recordid><startdate>20120520</startdate><enddate>20120520</enddate><creator>Mackey, Jonathan</creator><creator>MOHAMED, SHAZRENE</creator><creator>NEILSON, HILDING R</creator><creator>Langer, Norbert</creator><creator>Meyer, M-A</creator><scope>7TG</scope><scope>KL.</scope><scope>8FD</scope><scope>H8D</scope><scope>L7M</scope><scope>OTOTI</scope></search><sort><creationdate>20120520</creationdate><title>DOUBLE BOW SHOCKS AROUND YOUNG, RUNAWAY RED SUPERGIANTS: APPLICATION TO BETELGEUSE</title><author>Mackey, Jonathan ; MOHAMED, SHAZRENE ; NEILSON, HILDING R ; Langer, Norbert ; Meyer, M-A</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-o249t-49e0877ee85a81d4765d3cdb6257eb03275db76350326d53746eaac05928fa33</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2012</creationdate><topic>Astronomical models</topic><topic>ASTROPHYSICS</topic><topic>ASTROPHYSICS, COSMOLOGY AND ASTRONOMY</topic><topic>BINARY STARS</topic><topic>Computer simulation</topic><topic>Constants</topic><topic>Evolutionary</topic><topic>HERTZSPRUNG-RUSSELL DIAGRAM</topic><topic>HYDRODYNAMICS</topic><topic>INTERSTELLAR SPACE</topic><topic>MASS</topic><topic>RED GIANT STARS</topic><topic>Shells</topic><topic>SHOCK WAVES</topic><topic>STAR CLUSTERS</topic><topic>STAR EVOLUTION</topic><topic>Stars</topic><topic>STELLAR WINDS</topic><topic>Three dimensional</topic><topic>THREE-DIMENSIONAL CALCULATIONS</topic><topic>TWO-DIMENSIONAL CALCULATIONS</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Mackey, Jonathan</creatorcontrib><creatorcontrib>MOHAMED, SHAZRENE</creatorcontrib><creatorcontrib>NEILSON, HILDING R</creatorcontrib><creatorcontrib>Langer, Norbert</creatorcontrib><creatorcontrib>Meyer, M-A</creatorcontrib><collection>Meteorological & Geoastrophysical Abstracts</collection><collection>Meteorological & Geoastrophysical Abstracts - Academic</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Advanced Technologies Database with Aerospace</collection><collection>OSTI.GOV</collection><jtitle>Astrophysical journal. Letters</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Mackey, Jonathan</au><au>MOHAMED, SHAZRENE</au><au>NEILSON, HILDING R</au><au>Langer, Norbert</au><au>Meyer, M-A</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>DOUBLE BOW SHOCKS AROUND YOUNG, RUNAWAY RED SUPERGIANTS: APPLICATION TO BETELGEUSE</atitle><jtitle>Astrophysical journal. Letters</jtitle><date>2012-05-20</date><risdate>2012</risdate><volume>751</volume><issue>1</issue><spage>1</spage><epage>6</epage><pages>1-6</pages><issn>2041-8205</issn><eissn>2041-8213</eissn><abstract>A significant fraction of massive stars are moving supersonically through the interstellar medium (ISM), either due to disruption of a binary system or ejection from their parent star cluster. The interaction of their wind with the ISM produces a bow shock. In late evolutionary stages these stars may undergo rapid transitions from red to blue and vice versa on the Hertzsprung-Russell diagram, with accompanying rapid changes to their stellar winds and bow shocks. Recent three-dimensional simulations of the bow shock produced by the nearby runaway red supergiant (RSG) Betelgeuse, under the assumption of a constant wind, indicate that the bow shock is very young (<30,000 years old), hence Betelgeuse may have only recently become an RSG. To test this possibility, we have calculated stellar evolution models for single stars which match the observed properties of Betelgeuse in the RSG phase. The resulting evolving stellar wind is incorporated into two-dimensional hydrodynamic simulations in which we model a runaway blue supergiant (BSG) as it undergoes the transition to an RSG near the end of its life. We find that the collapsing BSG wind bubble induces a bow shock-shaped inner shell around the RSG wind that resembles Betelgeuse's bow shock, and has a similar mass. Surrounding this is the larger-scale retreating bow shock generated by the now defunct BSG wind's interaction with the ISM. We suggest that this outer shell could explain the bar feature located (at least in projection) just in front of Betelgeuse's bow shock.</abstract><cop>United States</cop><doi>10.1088/2041-8205/751/1/L10</doi><tpages>6</tpages></addata></record> |
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| subjects | Astronomical models ASTROPHYSICS ASTROPHYSICS, COSMOLOGY AND ASTRONOMY BINARY STARS Computer simulation Constants Evolutionary HERTZSPRUNG-RUSSELL DIAGRAM HYDRODYNAMICS INTERSTELLAR SPACE MASS RED GIANT STARS Shells SHOCK WAVES STAR CLUSTERS STAR EVOLUTION Stars STELLAR WINDS Three dimensional THREE-DIMENSIONAL CALCULATIONS TWO-DIMENSIONAL CALCULATIONS |
| title | DOUBLE BOW SHOCKS AROUND YOUNG, RUNAWAY RED SUPERGIANTS: APPLICATION TO BETELGEUSE |
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