T Tauri star magnetic fields and magnetospheres

Hussain, G. A. J.

doi:10.1002/asna.201111627

Cited by 13 publications

(16 citation statements)

References 80 publications

(88 reference statements)

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“…The exception is V2247 Oph, which possesses a highly complex and weak field but has too low a mass to develop a radiative core as it evolves. These results have been reviewed by Gregory & Donati (2011) and Hussain (2012). Similar results have been found for the sample of mainsequence M dwarfs that have been studied using ZDI (Donati et al 2008b;Morin et al 2008;Morin et al 2010), though for PMS stars, the situation is more complicated because the internal structure of PMS stars is determined by both mass and age .…”

Section: Introductionsupporting

confidence: 58%

Classical T Tauri stars: magnetic fields, coronae and star–disc interactions

Johnstone¹,

Jardine²,

Gregory³

et al. 2013

Monthly Notices of the Royal Astronomical Society

102

105

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The magnetic fields of young stars set their coronal properties and control their spin evolution via the star-disc interaction and outflows. Using 14 magnetic maps of 10 classical T Tauri stars (CTTSs) we investigate their closed X-ray emitting coronae, their open wind-bearing magnetic fields, and the geometry of magnetospheric accretion flows. The magnetic fields of all the CTTSs are multipolar. Stars with simpler (more dipolar) large-scale magnetic fields have stronger fields, are slower rotators, and have larger X-ray emitting coronae compared to stars with more complex large-scale magnetic fields. The field complexity controls the distribution of open and closed field regions across the stellar surface, and strongly influences the location and shapes of accretion hot spots. However, the higher order field components are of secondary importance in determining the total unsigned open magnetic flux, which depends mainly on the strength of the dipole component and the stellar surface area. Likewise, the dipole component alone provides an adequate approximation of the disc truncation radius. For some stars, the pressure of the hot coronal plasma dominates the stellar magnetic pressure and forces open the closed field inside the disc truncation radius. This is significant as accretion models generally assume that the magnetic field has a closed geometry out to the inner disc edge.

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Section: Introductionsupporting

confidence: 58%

Classical T Tauri stars: magnetic fields, coronae and star–disc interactions

Johnstone¹,

Jardine²,

Gregory³

et al. 2013

Monthly Notices of the Royal Astronomical Society

102

105

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“…In contrast to solar-type stars, both main-sequence stars below about 0.4 M ⊙ and T Tauri stars often display dipole fields of the order of 1 kG (e.g. [192–194] and references therein). Some recent results are summarized in figure 17.…”

Section: Interaction Between Convective and Radiative Zonesmentioning

confidence: 99%

“…In contrast to solar-type stars, both main-sequence stars below about 0.4 M and T Tauri stars often display dipole fields of the order of 1 kG (e.g. [192][193][194] [192,195,196], Donati et al [197] and Phan-Bao et al [198]. therein).…”

Section: Fully Convective Starsmentioning

confidence: 99%

Magnetic fields in non-convective regions of stars

Braithwaite

Spruit

2017

R. Soc. open sci.

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We review the current state of knowledge of magnetic fields inside stars, concentrating on recent developments concerning magnetic fields in stably stratified (zones of) stars, leaving out convective dynamo theories and observations of convective envelopes. We include the observational properties of A, B and O-type main-sequence stars, which have radiative envelopes, and the fossil field model which is normally invoked to explain the strong fields sometimes seen in these stars. Observations seem to show that Ap-type stable fields are excluded in stars with convective envelopes. Most stars contain both radiative and convective zones, and there are potentially important effects arising from the interaction of magnetic fields at the boundaries between them; the solar cycle being one of the better known examples. Related to this, we discuss whether the Sun could harbour a magnetic field in its core. Recent developments regarding the various convective and radiative layers near the surfaces of early-type stars and their observational effects are examined. We look at possible dynamo mechanisms that run on differential rotation rather than convection. Finally, we turn to neutron stars with a discussion of the possible origins for their magnetic fields.

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“…These are typical dynamo fields (e.g. Donati et al 2011, Johns-Krull et al 2011, and Hussain et al 2012, and they strongly affect how material is accreted onto the star.…”

Section: Pre-main Sequence Starsmentioning

confidence: 98%

Surface magnetic fields across the HR Diagram

Landstreet

2014

Proc. IAU

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The past 20 years have seen remarkable advances in spectropolarimetric instrumentation that have allowed us, for the first time, to identify some magnetic stars in most major stages of stellar evolution. We are beginning to see the broad outline of how such fields change during stellar evolution, to confront theoretical hypotheses and models of magnetic field structure and evolution with detailed data, and to understand more of the ways in which the presence of a field in turn affects stellar structure and evolution.

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T Tauri star magnetic fields and magnetospheres

Cited by 13 publications

References 80 publications

Classical T Tauri stars: magnetic fields, coronae and star–disc interactions

Classical T Tauri stars: magnetic fields, coronae and star–disc interactions

Magnetic fields in non-convective regions of stars

Surface magnetic fields across the HR Diagram

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