Mass Loss in Pre-main-sequence Stars via Coronal Mass Ejections and Implications for Angular Momentum Loss
dc.contributor.author | Aarnio, Alicia N. | en_US |
dc.contributor.author | Matt, Sean P. | en_US |
dc.contributor.author | Stassun, Keivan G. | en_US |
dc.date.accessioned | 2013-06-28T15:25:43Z | |
dc.date.available | 2013-06-28T15:25:43Z | |
dc.date.issued | 2012 | en_US |
dc.identifier.citation | Aarnio, Alicia N.; Matt, Sean P.; Stassun, Keivan G. (2012). "Mass Loss in Pre-main-sequence Stars via Coronal Mass Ejections and Implications for Angular Momentum Loss." The Astrophysical Journal 760(1): 9. <http://hdl.handle.net/2027.42/98581> | en_US |
dc.identifier.uri | http://stacks.iop.org/0004-637X/760/i=1/a=9 | en_US |
dc.identifier.uri | https://hdl.handle.net/2027.42/98581 | |
dc.description.abstract | We develop an empirical model to estimate mass-loss rates via coronal mass ejections (CMEs) for solar-type pre-main-sequence (PMS) stars. Our method estimates the CME mass-loss rate from the observed energies of PMS X-ray flares, using our empirically determined relationship between solar X-ray flare energy and CME mass: log ( M CME [g]) = 0.63 × log ( E flare [erg]) – 2.57. Using masses determined for the largest flaring magnetic structures observed on PMS stars, we suggest that this solar-calibrated relationship may hold over 10 orders of magnitude in flare energy and 7 orders of magnitude in CME mass. The total CME mass-loss rate we calculate for typical solar-type PMS stars is in the range 10 –12 -10 –9 M ☉ yr –1 . We then use these CME mass-loss rate estimates to infer the attendant angular momentum loss leading up to the main sequence. Assuming that the CME outflow rate for a typical ~1 M ☉ T Tauri star is <10 –10 M ☉ yr –1 , the resulting spin-down torque is too small during the first ~1 Myr to counteract the stellar spin-up due to contraction and accretion. However, if the CME mass-loss rate is ##IMG## [http://ej.iop.org/icons/Entities/gsim.gif] {gsim 10 –10 M ☉ yr –1 , as permitted by our calculations, then the CME spin-down torque may influence the stellar spin evolution after an age of a few Myr. | en_US |
dc.publisher | IOP Publishing | en_US |
dc.title | Mass Loss in Pre-main-sequence Stars via Coronal Mass Ejections and Implications for Angular Momentum Loss | en_US |
dc.type | Article | en_US |
dc.subject.hlbsecondlevel | Physics | en_US |
dc.subject.hlbtoplevel | Science | en_US |
dc.description.peerreviewed | Peer Reviewed | en_US |
dc.description.bitstreamurl | http://deepblue.lib.umich.edu/bitstream/2027.42/98581/1/0004-637X_760_1_9.pdf | |
dc.identifier.doi | 10.1088/0004-637X/760/1/9 | en_US |
dc.identifier.source | The Astrophysical Journal | en_US |
dc.owningcollname | Physics, Department of |
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