A non-extensive approach to the stellar rotational evolution – I: F- and G-type stars
The pioneering study by Skumanich showed that the rotational velocity of G-type mainsequence (MS) stars decreases with stellar age according to v sin i ∝ t −1/2. This relationship is consistent with simple theories of angular momentum loss from rotating stars, where an ionized wind is coupled to the...
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| Principais autores: | , |
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| Formato: | article |
| Idioma: | English |
| Publicado em: |
Oxford University Press
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| Endereço do item: | https://repositorio.ufrn.br/jspui/handle/123456789/29106 |
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| Resumo: | The pioneering study by Skumanich showed that the rotational velocity of G-type mainsequence (MS) stars decreases with stellar age according to v sin i ∝ t −1/2. This relationship is consistent with simple theories of angular momentum loss from rotating stars, where an ionized wind is coupled to the star by a magnetic field. The present study introduces a new approach to the study of stellar rotational braking in unsaturated F- and G-type stars limited in age and mass, connecting angular momentum loss by magnetic stellar wind with Tsallis non-extensive statistical mechanics. As a result, we show that the rotation–age relationship
can be well reproduced using a non-extensive approach from Tsallis non-extensive models.
Here, the index q, which is related to the degree of non-extensivity, can be associated with the
dynamo process and to magnetic field geometry, offering relevant information on the level of
stellar magnetic braking for F- and G-type MS stars. |
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