Modeling X-ray emission from stellar coronae

Costanza Argiroffi, Argiroffi, Jardine, Gregory, Donati

Risultato della ricerca: Paper

Abstract

By extrapolating from observationally derived surface magnetograms of low-mass stars we construct models of their coronal magnetic fields and compare the 3D field geometry with axial multipoles. AB Dor, which has a radiative core, has a very complex field, whereas V374 Peg, which is completely convective, has a simple dipolar field. We calculate global X-ray emission measures assuming that the plasma trapped along the coronal loops is in hydrostatic equilibrium and compare the differences between assuming isothermal coronae, or by considering a loop temperature profiles. Our preliminary results suggest that the non-isothermal model works well for the complex field of AB Dor, but not for the simple field of V374 Peg.
Lingua originaleEnglish
Stato di pubblicazionePublished - 2009

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stellar coronas
coronal loops
magnetic signatures
hydrostatics
temperature profiles
coronas
multipoles
x rays
stars
geometry
magnetic fields

All Science Journal Classification (ASJC) codes

  • Physics and Astronomy(all)

Cita questo

Argiroffi, C., Argiroffi, Jardine, Gregory, & Donati (2009). Modeling X-ray emission from stellar coronae.

Modeling X-ray emission from stellar coronae. / Argiroffi, Costanza; Argiroffi; Jardine; Gregory; Donati.

2009.

Risultato della ricerca: Paper

Argiroffi, C, Argiroffi, Jardine, Gregory & Donati 2009, 'Modeling X-ray emission from stellar coronae'.
Argiroffi C, Argiroffi, Jardine, Gregory, Donati. Modeling X-ray emission from stellar coronae. 2009.
Argiroffi, Costanza ; Argiroffi ; Jardine ; Gregory ; Donati. / Modeling X-ray emission from stellar coronae.
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abstract = "By extrapolating from observationally derived surface magnetograms of low-mass stars we construct models of their coronal magnetic fields and compare the 3D field geometry with axial multipoles. AB Dor, which has a radiative core, has a very complex field, whereas V374 Peg, which is completely convective, has a simple dipolar field. We calculate global X-ray emission measures assuming that the plasma trapped along the coronal loops is in hydrostatic equilibrium and compare the differences between assuming isothermal coronae, or by considering a loop temperature profiles. Our preliminary results suggest that the non-isothermal model works well for the complex field of AB Dor, but not for the simple field of V374 Peg.",
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AU - Argiroffi, Costanza

AU - Argiroffi, null

AU - Jardine, null

AU - Gregory, null

AU - Donati, null

PY - 2009

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N2 - By extrapolating from observationally derived surface magnetograms of low-mass stars we construct models of their coronal magnetic fields and compare the 3D field geometry with axial multipoles. AB Dor, which has a radiative core, has a very complex field, whereas V374 Peg, which is completely convective, has a simple dipolar field. We calculate global X-ray emission measures assuming that the plasma trapped along the coronal loops is in hydrostatic equilibrium and compare the differences between assuming isothermal coronae, or by considering a loop temperature profiles. Our preliminary results suggest that the non-isothermal model works well for the complex field of AB Dor, but not for the simple field of V374 Peg.

AB - By extrapolating from observationally derived surface magnetograms of low-mass stars we construct models of their coronal magnetic fields and compare the 3D field geometry with axial multipoles. AB Dor, which has a radiative core, has a very complex field, whereas V374 Peg, which is completely convective, has a simple dipolar field. We calculate global X-ray emission measures assuming that the plasma trapped along the coronal loops is in hydrostatic equilibrium and compare the differences between assuming isothermal coronae, or by considering a loop temperature profiles. Our preliminary results suggest that the non-isothermal model works well for the complex field of AB Dor, but not for the simple field of V374 Peg.

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