Dynamo processes and activity cycles of the active stars AB Doradus, LQ Hydrae and HR 1099

By J. Donati, A. Cameron, M. Semel, G. Hussain, P. Petit, B. Carter, S. Marsden, M. Mengel, A. Ariste, S. Jeffers and 1 more. 2003

227 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/13042cbb44e3b40e5bc097a4bd4ad7f873a19a51

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In Astronomy and Astrophysics

1. A. Reiners
2. J. Donati
3. J. Landstreet
4. S. Cranmer
5. N. Piskunov
6. M. Gudel
7. J. Morin
8. J. Bouvier

Citations in the corpus

• The Sun in Time: Activity and Environment (2007, background): “Initial results were presented in Dorren et al. (1995), a more complete time series has been published by Güdel (2004).”
• Large-scale magnetic topologies of late M dwarfs⋆ (2008, methodology): “This is at odds with what is observed in more massive active stars, whose magnetic fields reportedly evolve significantly on time-scales of only a few months (e.g., Donati et al. 2003a).”
• Toroidal versus poloidal magnetic fields in Sun-like stars: a rotation threshold (2008, background): “…on a few objects quite different from the Sun by their mass (Valenti, Marcy & Basri 1995; Reiners & Basri 2007) or rotation rate (Rüedi et al. 1997; Donati et al. 2003; Petit et al. 2005), measurements of Zeeman signatures have always failed at detecting the magnetic field of low-activity solar…”
• Magnetic Fields of Nondegenerate Stars (2009, methodology): “A well defined minimum at physically sensible values ofΩeq anddΩ suggests that differential rotation is present at the surface of the star (e.g., Donati et al. 2003b).”
• A BCool magnetic snapshot survey of solar-type stars (2013, background): “A significant amount of work has previously been achieved using spectropolarimetric observations of young, active, solar-type stars (i.e. Donati et al. 1997, 2003; Jeffers et al. 2011; Marsden et al. 2011a,b), but it is only with recent advances in instrumentation, such as the development of the…”
• Magnetospheric accretion on the T Tauri star BP Tauri (2008, background): “…at triggering strong nearly-axisymmetric low-order poloidal surface magnetic topologies (Donati et al. 2006a; Hallinan et al. 2006; Morin et al. 2007; Hallinan et al. 2007, Morin et al., 2008 in preparation) than their more massive partly-convective counterparts (e.g., Donati et al. 2003).”
• Large-scale magnetic topologies of early M dwarfs (2008, background): “Thanks to time-resolved spectropolarimetric observations of cool stars, we are now able to recover information on how magnetic fields distribute at (and emerge from) the surfaces of cool active stars (e.g., Donati et al. 2003a).”
• A multiwavelength study of the M dwarf binary YY Geminorum (2015, background): “Other indications on surface structure however, such as come from the more detailed Zeeman Doppler Imaging techniques for example (Donati et al, 2003), tend to support somewhat simple and uniform structures to maculae, and there are supporting theoretical arguments, related to magnetic loop…”
• A high-resolution spectropolarimetric survey of Herbig Ae/Be stars – I. Observations and measurements (2012, background): “…as part of parallel observational programs with ESPaDOnS, Narval and FORS1 on the Very Large Telescope (ESO, Chile), or the Semel Polarimeter (SEMPOL; Semel 1989; Semel, Donati & Rees 1993; Donati et al. 2003) coupled with the spectrograph UCLES on the Anglo Australian Telescope (AAT, Australia).”
• Magnetic fields and accretion flows on the classical T Tauri star V2129 Oph (2007, methodology): “The photospheric Stokes I profiles exhibit shape variations reminiscent of the distortions induced by cool surface spots in spectral lines of active stars (e.g., Donati et al. 2003).”
• Magnetic cycles of the planet-hosting star τ Bootis (2008, methodology): “To incorporate differential rotation into the modelling, we proceed as in Donati et al. (2003) and Morin et al. (2007), i.e., by assuming that the rotation rate at the surface of the star is varying with latitude θ as Ωeq − dΩsin 2 θ where Ωeq is the rotation rate at the equator dΩ the difference…”
• Least-squares deconvolution of the stellar intensity and polarization spectra (2010, methodology): “…the latter investigations the time series of theLSD profiles were interpreted under different physical assumptions, with regularized inversion techniques to produce magnetic( .g., Donati et al. 2003), chemical (Folsom et al. 2008), and brightness (e.g., Jeffers et al. 2007) maps of stellar surface.”
• Self-consistent Coronal Heating and Solar Wind Acceleration from Anisotropic Magnetohydrodynamic Turbulence (2007, methodology): “Observational determinations of the field geometries of rapidly rotating young stars have been made possible via Zeeman-Doppler imaging (e.g., Donati et al. 1990, 2003), time-resolved X-ray spectroscopy (Hussain et al. 2005), and combinations of these and related techniques.”
• Stellar magnetism: empirical trends with age and rotation (2014, unknown): “The magnetic maps, 104 in total, have either been published elsewhere (Donati et al. 1999, 2003, 2008a,c,b, 2010a,b, 2011a,b,c, 2012, 2013; Marsden et al. 2006, 2011; Catala et al. 2007; Morin et al. 2008a,b, 2010; Petit et al. 2008, 2009; Hussain et al. 2009; Fares et al. 2009, 2010, 2012, 2013;…”
• The surprising magnetic topology of τ Sco: fossil remnant or dynamo output? (2006, unknown): “In particular, we note that, compared to the potential component, this toroidal component is much weaker in τ Sco than in most cool magnetic stars observed to date, where the toroidal component largely exceeded the poloidal one (e.g., Donati et al. 2003).”