Inferring the sun's internal angular velocity from observed p-mode frequency splittings

Brown, Timothy M.; Christensen‐Dalsgaard, J.; Dziembowski, W. A.; Goode, Philip R.; Gough, D. O.; Morrow, C. A.

doi:10.1086/167727

Cited by 338 publications

(201 citation statements)

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“…This expectation is not supported by measurements of internal solar rotation (Brown et al 1989). According to the above interpretation, the difference in the angular velocity between the Sun's radiative core and its convective envelope must thus have been erased by some mechanism of angular momentum redistribution.…”

Section: Discussionmentioning

confidence: 83%

X-ray emission regimes and rotation sequences in M 35

Gondoin

2013

A&A

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Context. Late-type stars in young open clusters show two kinds of dependence of their X-ray emission on rotation. They also tend to group into two main sub-populations that lie on narrow sequences in diagrams where their rotation periods are plotted against their (B − V) colour indices. A correlation between these two regimes of X-ray emission and the rotation sequences has been recently observed in the M 34 open cluster. Sun-like M 34 stars also show a drop of their X-ray to bolometric luminosity ratio by about one order of magnitude at a Rossby number of about 0.3. Aims. The present study looks for similar connections between X-ray activity and rotation in an other open cluster. The aim is to consolidate a model of X-ray activity evolution on the main sequence and to provide observational constraints on dynamo processes in the interiors of late-type stars. Methods. The paper compares XMM-Newton measurements of X-ray stellar emission in M 35 with X-ray luminosity distributions derived from rotation period measurements assuming either an X-ray regime transition at a critical Rossby number or a correlation between X-ray emission regimes and rotation sequences. Results. This second hypothesis could account for the low number of M 35 stars detected in X-rays. A model of X-ray activity evolution is proposed based on the correlation. One major output is that the transition from saturated to non-saturated X-ray emission occurs at Rossby numbers between about 0.13 and 0.4 for each star depending on its mass and initial period of rotation on the ZAMS. This prediction agrees with observations of stellar X-ray emission in M 34. It explains the large range of X-ray luminosities observed among Sun-like stars in young open clusters. Conclusions. I conclude that the correlation between X-ray emission regimes and rotation sequences could be a fundamental property of the early evolution of stellar magnetic activity on the main sequence. I argue that the angular momentum redistribution mechanism(s) responsible for the transition between rotation sequences could result in a changing mixture of dynamo processes occurring side by side, possibly including a turbulent dynamo at high rotation rate and an interface-type dynamo whose efficiency decreases progressively at later stage of stellar evolution when rotation dies away.

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Section: Discussionmentioning

confidence: 83%

X-ray emission regimes and rotation sequences in M 35

Gondoin

2013

A&A

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“…The convective envelopes of the subgiants and giants have deepened and dredged up material from the interior of the stars and thus provide a view of the internal composition. Many observations show that subgiant stars originating from this side of the dip present a large range of lithium abundances that cannot be explained by standard dilution alone (Alschuler 1975;Brown et al 1989;Balachandran 1990;do Nascimento et al 2000). These observations suggest that a lithium depletion process takes place in the radiative interior during the main-sequence phase, even if its effects are not visible at the surface at the age of the Hyades (Vauclair 1991;).…”

Section: The Lithium Dipmentioning

confidence: 99%

On the Coupling between Helium Settling and Rotation‐induced Mixing in Stellar Radiative Zones. III. Applications to Light Elements in Population I Main‐Sequence Stars

Théado

Vauclair

2003

ApJ

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In the two previous papers of this series, we have discussed the importance of the l-gradients due to helium settling in rotation-induced mixing, first in an approximate analytical way, second in a two-dimensional numerical simulation. We have found that, for slowly rotating low-mass stars, a process of '' creeping paralysis,'' in which the circulation and the diffusion are nearly frozen, may take place below the convective zone. Here we apply this theory to the case of lithium and beryllium in Galactic clusters, especially the Hyades. We take into account the rotational braking with rotation velocities adjusted to the present observations. We find that two different cells of meridional circulation appear on the hot side of the '' lithium dip '' and that the creeping paralysis process occurs, not directly below the convective zone, but deeper inside the radiative zone, at the top of the second cell. As a consequence, the two cells are disconnected, which may be the basic reason for the lithium increase with effective temperature on this side of the dip. On the cool side, there is just one cell of circulation, and the paralysis has not yet set in at the age of the Hyades; the same modeling accounts nicely for the beryllium observations as well as for the lithium ones.

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“…Using an ingenious observational technique, obtained rotational splittings of sectoral modes; the analysis of these data by showed no indication of rapid rotation of the radiative interior, even quite close to the solar centre. Also, the initial observations and analyses of the m dependence of rotational splittings (e.g., Brown & Morrow 1987;Christensen-Dalsgaard & Schou 1988;Libbrecht 1988;Brown et al 1989) indicated that rotation in the convection zone was roughly independent of depth, with a transition near the base of the convection zone to nearly uniform rotation in the radiative interior; this was quite unlike the rotation on cylinders predicted theoretically.…”

Section: The Solar Internal Rotationmentioning

confidence: 95%

The Internal Solar Rotation from Helioseismology

Christensen‐Dalsgaard

2004

Symp. - Int. Astron. Union

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Helioseismology has provided detailed inferences about the internal rotation of the Sun, and hence stringent constraints on any attempt to understand the properties and evolution of stellar rotation. Here I briefly discuss the techniques used in the analysis and review the results that have been obtained. Strikingly, these results are markedly different from the predictions made before the helioseismic data became available, emphasizing the difficulties in the modelling of phenomena as complex as stellar internal rotation.

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Inferring the sun's internal angular velocity from observed p-mode frequency splittings

Cited by 338 publications

References 0 publications

X-ray emission regimes and rotation sequences in M 35

X-ray emission regimes and rotation sequences in M 35

On the Coupling between Helium Settling and Rotation‐induced Mixing in Stellar Radiative Zones. III. Applications to Light Elements in Population I Main‐Sequence Stars

The Internal Solar Rotation from Helioseismology

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