The Interaction of Rotation and Magnetic Field in the Solar System
During the early phases of star formation, torsional Alfven waves propagating along the locally distorted galactic magnetic field can transport away the bulk of the initial angular momentum of a condensation, so enabling it to contract to solar nebula dimensions. Enough primeval magnetic flux may be...
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| Veröffentlicht in: | Philosophical transactions of the Royal Society of London. Series A: Mathematical and physical sciences 1984-11, Vol.313 (1524), p.19-25 |
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| container_issue | 1524 |
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| container_title | Philosophical transactions of the Royal Society of London. Series A: Mathematical and physical sciences |
| container_volume | 313 |
| creator | Mestel, L. |
| description | During the early phases of star formation, torsional Alfven waves propagating along the locally distorted galactic magnetic
field can transport away the bulk of the initial angular momentum of a condensation, so enabling it to contract to solar nebula
dimensions. Enough primeval magnetic flux may be retained for magnetic redistribution of angular momentum to continue until
the proto-Sun reaches the pre-Main Sequence Hayashi phase. A rotating star with a convective envelope has a dynamo-maintained
field which brakes the star through coupling to the stellar wind. Observational evidence from young star clusters and from
T Tauri stars suggests that the zero-age Main Sequence Sun had about ten times its present angular momentum. The same braking
process, scaled up because of the much more powerful T Tauri winds, can explain why the zero-age Sun had lost at least nine-tenths
of the centrifugal upper limit, and is more acceptable than the suggestion that the `missing' solar angular momentum has been
magnetically fed into the planetary system. |
| doi_str_mv | 10.1098/rsta.1984.0079 |
| format | Article |
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field can transport away the bulk of the initial angular momentum of a condensation, so enabling it to contract to solar nebula
dimensions. Enough primeval magnetic flux may be retained for magnetic redistribution of angular momentum to continue until
the proto-Sun reaches the pre-Main Sequence Hayashi phase. A rotating star with a convective envelope has a dynamo-maintained
field which brakes the star through coupling to the stellar wind. Observational evidence from young star clusters and from
T Tauri stars suggests that the zero-age Main Sequence Sun had about ten times its present angular momentum. The same braking
process, scaled up because of the much more powerful T Tauri winds, can explain why the zero-age Sun had lost at least nine-tenths
of the centrifugal upper limit, and is more acceptable than the suggestion that the `missing' solar angular momentum has been
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field can transport away the bulk of the initial angular momentum of a condensation, so enabling it to contract to solar nebula
dimensions. Enough primeval magnetic flux may be retained for magnetic redistribution of angular momentum to continue until
the proto-Sun reaches the pre-Main Sequence Hayashi phase. A rotating star with a convective envelope has a dynamo-maintained
field which brakes the star through coupling to the stellar wind. Observational evidence from young star clusters and from
T Tauri stars suggests that the zero-age Main Sequence Sun had about ten times its present angular momentum. The same braking
process, scaled up because of the much more powerful T Tauri winds, can explain why the zero-age Sun had lost at least nine-tenths
of the centrifugal upper limit, and is more acceptable than the suggestion that the `missing' solar angular momentum has been
magnetically fed into the planetary system.</description><subject>Angular momentum</subject><subject>Astronomy</subject><subject>Average linear density</subject><subject>Braking</subject><subject>Earth, ocean, space</subject><subject>Exact sciences and technology</subject><subject>Magnetic fields</subject><subject>Magnetic flux</subject><subject>Mass</subject><subject>Rotating generators</subject><subject>Solar physics</subject><subject>Solar system</subject><subject>Solar systems</subject><subject>Sun</subject><subject>T Tauri stars</subject><issn>1364-503X</issn><issn>0080-4614</issn><issn>1471-2962</issn><issn>2054-0272</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>1984</creationdate><recordtype>article</recordtype><recordid>eNp9Uk1v1DAUjBBIlMKVA6ccELds_WznwxekUlGoVITUXSRu1otjd73KxovtgJZfj5NUFRWiJz_LM_NmRs6y10BWQERz5kPEFYiGrwipxZPsBHgNBRUVfZpmVvGiJOz78-xFCDtCAKqSnmQfNludXw1Re1TRuiF3Jr9xEecZhy7_greDjlbll1b3XW6HPCbG2vXo8_UxRL1_mT0z2Af96u48zb5dftxcfC6uv366uji_LhQXZSw6rClXaDRXAG3TEiZKgQZaIzBZodSYBruqaknL644DNoqQktS8pgSZYOw0e7foHrz7MeoQ5d4GpfseB-3GICnnpagEJOBqASrvQvDayIO3e_RHCUROVcmpKjlVJaeqEuHtnTIGhb3xOCgb7lmCQNVUEywsMO-OKahTVsej3LnRD-kqb9abcxCM_2TALJQ0iTcMCAfKqfxtD_PWCSATQNoQRi1n2EM3_5pjj239b6Q3C2sXovP3UVhdzUHOlsetvd3-sl7LB9rpckhik8vZH0yM948ypuXKpW80xL950ox9Lw-dYX8AZBTPew</recordid><startdate>19841127</startdate><enddate>19841127</enddate><creator>Mestel, L.</creator><general>The Royal Society</general><general>Royal Society of London</general><scope>IQODW</scope><scope>AAYXX</scope><scope>CITATION</scope><scope>8FD</scope><scope>H8D</scope><scope>L7M</scope></search><sort><creationdate>19841127</creationdate><title>The Interaction of Rotation and Magnetic Field in the Solar System</title><author>Mestel, L.</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c495t-da724cafe4c11b8b03959af1bf9a65222ff8ad66b0b47d41a8c005074720a3933</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>1984</creationdate><topic>Angular momentum</topic><topic>Astronomy</topic><topic>Average linear density</topic><topic>Braking</topic><topic>Earth, ocean, space</topic><topic>Exact sciences and technology</topic><topic>Magnetic fields</topic><topic>Magnetic flux</topic><topic>Mass</topic><topic>Rotating generators</topic><topic>Solar physics</topic><topic>Solar system</topic><topic>Solar systems</topic><topic>Sun</topic><topic>T Tauri stars</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Mestel, L.</creatorcontrib><collection>Pascal-Francis</collection><collection>CrossRef</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Advanced Technologies Database with Aerospace</collection><jtitle>Philosophical transactions of the Royal Society of London. Series A: Mathematical and physical sciences</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Mestel, L.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>The Interaction of Rotation and Magnetic Field in the Solar System</atitle><jtitle>Philosophical transactions of the Royal Society of London. Series A: Mathematical and physical sciences</jtitle><stitle>Phil. Trans. R. Soc. Lond. A</stitle><date>1984-11-27</date><risdate>1984</risdate><volume>313</volume><issue>1524</issue><spage>19</spage><epage>25</epage><pages>19-25</pages><issn>1364-503X</issn><issn>0080-4614</issn><eissn>1471-2962</eissn><eissn>2054-0272</eissn><coden>PTRMAD</coden><abstract>During the early phases of star formation, torsional Alfven waves propagating along the locally distorted galactic magnetic
field can transport away the bulk of the initial angular momentum of a condensation, so enabling it to contract to solar nebula
dimensions. Enough primeval magnetic flux may be retained for magnetic redistribution of angular momentum to continue until
the proto-Sun reaches the pre-Main Sequence Hayashi phase. A rotating star with a convective envelope has a dynamo-maintained
field which brakes the star through coupling to the stellar wind. Observational evidence from young star clusters and from
T Tauri stars suggests that the zero-age Main Sequence Sun had about ten times its present angular momentum. The same braking
process, scaled up because of the much more powerful T Tauri winds, can explain why the zero-age Sun had lost at least nine-tenths
of the centrifugal upper limit, and is more acceptable than the suggestion that the `missing' solar angular momentum has been
magnetically fed into the planetary system.</abstract><cop>London</cop><pub>The Royal Society</pub><doi>10.1098/rsta.1984.0079</doi><tpages>7</tpages></addata></record> |
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| ispartof | Philosophical transactions of the Royal Society of London. Series A: Mathematical and physical sciences, 1984-11, Vol.313 (1524), p.19-25 |
| issn | 1364-503X 0080-4614 1471-2962 2054-0272 |
| language | eng |
| recordid | cdi_pascalfrancis_primary_9016869 |
| source | JSTOR Mathematics & Statistics; Jstor Complete Legacy |
| subjects | Angular momentum Astronomy Average linear density Braking Earth, ocean, space Exact sciences and technology Magnetic fields Magnetic flux Mass Rotating generators Solar physics Solar system Solar systems Sun T Tauri stars |
| title | The Interaction of Rotation and Magnetic Field in the Solar System |
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