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Titolo:
First results on pre-main-sequence evolution, including a magnetic field
Autore:
DAntona, F; Ventura, P; Mazzitelli, I;
Indirizzi:
Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy Osservatorio Astron Roma Monte Porzio Catone Italy I-00040 Catone, Italy CNR, Ist Astrofis Spaziale, I-00133 Rome, Italy CNR Rome Italy I-00133CNR, Ist Astrofis Spaziale, I-00133 Rome, Italy
Titolo Testata:
ASTROPHYSICAL JOURNAL
fascicolo: 1, volume: 543, anno: 2000,
parte:, 2
pagine: L77 - L80
SICI:
0004-637X(20001101)543:1<L77:FROPEI>2.0.ZU;2-5
Fonte:
ISI
Lingua:
ENG
Soggetto:
STELLAR TURBULENT CONVECTION; LOW-MASS; STARS; MODEL; TAURI;
Keywords:
stars : fundamental parameters; stars : interiors; stars : magnetic fields; stars : pre-main-sequence;
Tipo documento:
Article
Natura:
Periodico
Settore Disciplinare:
Physical, Chemical & Earth Sciences
Citazioni:
21
Recensione:
Indirizzi per estratti:
Indirizzo: D'Antona, F Osservatorio Astron Roma, Via Frascati 33, I-00040 Monte Porzio Catone, Italy Osservatorio Astron Roma Via Frascati 33 Monte Porzio Catone Italy I-00040
Citazione:
F. D'Antona et al., "First results on pre-main-sequence evolution, including a magnetic field", ASTROPHYS J, 543(1), 2000, pp. L77-L80

Abstract

The recent preliminary determination of masses and physical parameters forthe ROSAT-discovered, weak T Tauri star RX J0529.4+0041, a double-lined eclipsing binary, is a very important test for the pre-main-sequence (PMS) models. In fact, its secondary (0.95 +/- 0.05 M.) is still in the Hayashi phase, where the effective temperatures (T-eff) are highly dependent on the modeling of the surface convective layers. We present new models for the PMS,including zero-order thermal modifications that are due to the magnetic field, generated by the dynamo that is due to the coupling between rotation and convection. This generally neglected physical input affects the T-eff location of the PMS: tracks that do not allow for the effect of the magnetic field on the convective gradients provide an upper limit to the T-eff. The present models can match the H-R diagram location of the secondary of RX J0529.4+0041 and the low lithium depletion expected for stars of similar to1 M.. We show that this new feature in the computation is not equivalent to an artificial parametric change of the convection efficiency. We also point out that more complete models are needed, including a self-consistency model between the dynamo magnetic field and the evolution of stellar rotation.

ASDD Area Sistemi Dipartimentali e Documentali, Università di Bologna, Catalogo delle riviste ed altri periodici
Documento generato il 05/12/20 alle ore 08:06:06