On a stochastic model for the spin-down of solar-type stars

Nicolas Leprovost; Eun Jin Kim

doi:10.1088/0004-637X/719/1/287

On a stochastic model for the spin-down of solar-type stars

Nicolas Leprovost, Eun Jin Kim

University of Sheffield

Research output: Contribution to journal › Article › peer-review

2 Citations (Scopus)

28 Downloads (Pure)

Abstract

Modeling the rotation history of solar-type stars is an outstanding problem in modern astrophysics. One of the main challenges is to explain the dispersion in the distribution of stellar rotation rate for young stars. Previous works have advocated diverse mechanisms to explain the presence of fast rotators (FRs) and also of slow rotators (SRs). For instance, dynamo saturation can limit the stellar spin-down and explain the presence of FRs but does not produce enough SRs. Here, we present a new model that can account for the presence of both types of rotators by incorporating fluctuations in the angular momentum loss. This renders the spin-down problem probabilistic in nature, some stars experiencing more braking on average than others. We show that random fluctuations in the loss of angular momentum enhance the population of both FR and SR compared to the deterministic cases (with a linear dynamo prescription or with dynamo saturation). The stochastic angular momentum loss thus provides an alternative physical mechanism to that of a saturated dynamo, with an even better agreement with observations.

Original language	English
Pages (from-to)	287-298
Number of pages	12
Journal	Astrophysical Journal
Volume	719
Issue number	1
DOIs	https://doi.org/10.1088/0004-637X/719/1/287
Publication status	Published - 19 Jul 2010
Externally published	Yes

Bibliographical note

Copyright © and Moral Rights are retained by the author(s) and/ or other copyright owners. A copy can be downloaded for personal non-commercial research or study, without prior permission or charge. This item cannot be reproduced or quoted extensively from without first obtaining permission in writing from the copyright holder(s). The content must not be changed in any way or sold commercially in any format or medium without the formal permission of the copyright holders.

Keywords

Stars: Evolution
Stars: Interiors
Stars: Rotation

ASJC Scopus subject areas

Space and Planetary Science
Astronomy and Astrophysics
Nuclear and High Energy Physics

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10.1088/0004-637X/719/1/287

PublishedFinal published version, 1.01 MBLicence: Unspecified

Cite this

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abstract = "Modeling the rotation history of solar-type stars is an outstanding problem in modern astrophysics. One of the main challenges is to explain the dispersion in the distribution of stellar rotation rate for young stars. Previous works have advocated diverse mechanisms to explain the presence of fast rotators (FRs) and also of slow rotators (SRs). For instance, dynamo saturation can limit the stellar spin-down and explain the presence of FRs but does not produce enough SRs. Here, we present a new model that can account for the presence of both types of rotators by incorporating fluctuations in the angular momentum loss. This renders the spin-down problem probabilistic in nature, some stars experiencing more braking on average than others. We show that random fluctuations in the loss of angular momentum enhance the population of both FR and SR compared to the deterministic cases (with a linear dynamo prescription or with dynamo saturation). The stochastic angular momentum loss thus provides an alternative physical mechanism to that of a saturated dynamo, with an even better agreement with observations.",

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N1 - Copyright © and Moral Rights are retained by the author(s) and/ or other copyright owners. A copy can be downloaded for personal non-commercial research or study, without prior permission or charge. This item cannot be reproduced or quoted extensively from without first obtaining permission in writing from the copyright holder(s). The content must not be changed in any way or sold commercially in any format or medium without the formal permission of the copyright holders.

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N2 - Modeling the rotation history of solar-type stars is an outstanding problem in modern astrophysics. One of the main challenges is to explain the dispersion in the distribution of stellar rotation rate for young stars. Previous works have advocated diverse mechanisms to explain the presence of fast rotators (FRs) and also of slow rotators (SRs). For instance, dynamo saturation can limit the stellar spin-down and explain the presence of FRs but does not produce enough SRs. Here, we present a new model that can account for the presence of both types of rotators by incorporating fluctuations in the angular momentum loss. This renders the spin-down problem probabilistic in nature, some stars experiencing more braking on average than others. We show that random fluctuations in the loss of angular momentum enhance the population of both FR and SR compared to the deterministic cases (with a linear dynamo prescription or with dynamo saturation). The stochastic angular momentum loss thus provides an alternative physical mechanism to that of a saturated dynamo, with an even better agreement with observations.

AB - Modeling the rotation history of solar-type stars is an outstanding problem in modern astrophysics. One of the main challenges is to explain the dispersion in the distribution of stellar rotation rate for young stars. Previous works have advocated diverse mechanisms to explain the presence of fast rotators (FRs) and also of slow rotators (SRs). For instance, dynamo saturation can limit the stellar spin-down and explain the presence of FRs but does not produce enough SRs. Here, we present a new model that can account for the presence of both types of rotators by incorporating fluctuations in the angular momentum loss. This renders the spin-down problem probabilistic in nature, some stars experiencing more braking on average than others. We show that random fluctuations in the loss of angular momentum enhance the population of both FR and SR compared to the deterministic cases (with a linear dynamo prescription or with dynamo saturation). The stochastic angular momentum loss thus provides an alternative physical mechanism to that of a saturated dynamo, with an even better agreement with observations.

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On a stochastic model for the spin-down of solar-type stars

Abstract

Bibliographical note

Keywords

ASJC Scopus subject areas

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