Magnetic Fields of Nondegenerate Stars

By J. Donati, J. Landstreet. 2009

534 citations recorded by the source corpus.

Magnetic fields are present in a wide variety of stars throughout the HR diagram and play a role at basically all evolutionary stages, from very-low-mass dwarfs to very massive stars, and from young star-forming molecular clouds and protostellar accretion discs to evolved giants/supergiants and magnetic white dwarfs/neutron stars. These fields range from a few μG (e.g., in molecular clouds) to TG and more (e.g., in magnetic neutron stars); in nondegenerate stars in particular, they feature large-scale topologies varying from simple nearly axisymmetric dipoles to complex nonaxsymmetric structures, and from mainly poloidal to mainly toroidal topologies. After recalling the main techniques of detecting and modeling stellar magnetic fields, we review the existing properties of magnetic fields reported in cool, hot, and young nondegenerate stars and protostars, and discuss our understanding of the origin of these fields and their impact on the birth and life of stars.

Subfields: Astronomy and Astrophysics, Instrumentation, Statistical and Nonlinear Physics

View Paper: https://www.semanticscholar.org/paper/4cccbe7a8accd2e5beecb0192249c104fb163a62

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In Astronomy and Astrophysics

1. Selma de Mink
2. A. Reiners
3. N. Langer
4. Robert G. Izzard
5. K. Luhman
6. G. Herczeg
7. J. Bouvier
8. J. Owen

In Instrumentation

1. Selma de Mink
2. N. Langer
3. A. Reiners
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5. J. Bouvier
6. G. Herczeg
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8. J. Owen

In Statistical and Nonlinear Physics

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2. R. Townsend
3. C. Knigge
4. G. Herczeg
5. Matteo Cantiello
6. Dean M. Townsley
7. P. Marchant
8. A. Reiners

Citations in the corpus

• Improved angular momentum evolution model for solar-like stars II. Exploring the mass dependence (2015, unknown): “…magnetic topology is indeed suggested for main-sequence stars, with solar-mass stars having more multipolar magnetic structure than lower mass stars whose magnetic topology tends to be dipole dominated (Petit et al. 2008; Donati & Landstreet 2009; Morin et al. 2010; Gregory et al. 2012).”
• The FIP and Inverse FIP Effects in Solar and Stellar Coronae (2015, background): “(2012) and Wood and Laming (2013), respectively, and αCen B from Drake et al. (1997). Diamonds indicate measurements from Telleschi et al. (2005), triangles from Liefke et al. (2008), with a solar value from Feldman and Laming (2000).”
• THE INCIDENCE OF STELLAR MERGERS AND MASS GAINERS AMONG MASSIVE STARS (2013, background): “For example, the fraction of massive stars that are observed to be magnetic stars , i.e. about 10%, (Donati & Landstreet 2009; Hubrig et al. 2011, 2013; Wade et al. 2011; Grunhut et al. 2012) is in the same order as the fraction of merger products that we expect.”
• The coronal X-ray - age relation and its implications for the evaporation of exoplanets (2011, background): “The efficiency of these mechanisms is determined by the interaction between convection in the outer envelope and differential rotation (e.g. Landstreet 1992; Covas, Moss &Tavakol 2005; Donati & Landstreet 2009).”
• The Effect of Stellar Rotation on Colour-Magnitude Diagrams: On the apparent presence of multiple populations in intermediate age stellar clusters (2009, background): “For example, in solar-type stars in our own galaxy magnetic fields are detected up to ∼ 1.5M⊙(Donati & Landstreet 2009).”
• RADIUS-DEPENDENT ANGULAR MOMENTUM EVOLUTION IN LOW-MASS STARS. I (2011, background): “Given that mulipole orders higher than radial are indeed broadly consistent with field configuration data at all stellar masses (e.g., Donati & Landstreet 2009), the latter solution must be important at some level, regardless of additional variations in KV and Ṁ .”
• THE MASS-DEPENDENCE OF ANGULAR MOMENTUM EVOLUTION IN SUN-LIKE STARS (2014, background): “…stars (Wood et al. 2005), theoretical predictions of wind properties (Suzuki et al. 2012; Cranmer & Saar 2011), mapping of surface magnetic fields (Donati & Landstreet 2009), and dynamo models (Miesch & Toomre 2009; Brun et al. 2014), we are still working to understand how these properties depend…”
• MODULES FOR EXPERIMENTS IN STELLAR ASTROPHYSICS (MESA): BINARIES, PULSATIONS, AND EXPLOSIONS (2015, background): “Similarly, magnetic fields in stars with radiative envelopes are of a significantly different nature than those seen in stars with convective envelopes, and there is no simple way to predict even the presence of magnetism (Donati & Landstreet 2009).”
• THE ROTATION RATES OF MASSIVE STARS: THE ROLE OF BINARY INTERACTION THROUGH TIDES, MASS TRANSFER, AND MERGERS (2012, background): “The fraction of more massive stars that show evidence for a magnetic field appears, however, to be smaller than about 15% (Donati & Landstreet 2009; Wade et al. 2012b).”
• The VLT-FLAMES Tarantula Survey XXVII. Physical parameters of B-type main-sequence binary systems in the Tarantula nebula (2017, unknown): “More recently it has been recognised that magnetic fields (Donati & Landstreet 2009) can a ff ect the internal structure and rotation profile, which in turn can a ff ect chemical mixing.”
• Observations of Cool-Star Magnetic Fields (2012, background): “Furthermore, Zeeman Doppler maps suggest that large-scale fields in classical T Tauri stars can undergo secular variations on timescales of a few years (e.g., Donati and Landstreet, 2009; Donati et al., 2011a).”
• Stellar magnetism: empirical trends with age and rotation (2014, methodology): “In the past decade, ZDI has been used to reconstruct the topology and intensity of the surface magnetic fields of roughly one hundred stars (for a recent review of the survey, see Donati & Landstreet 2009).”
• Cosmological Magnetic Fields: Their Generation, Evolution and Observation (2013, background): “Wherever we have the means of observing them, they are present: in our solar system, in stars (Donati and Landstreet 2009), in the Milky Way (Wielebinski 2005) in other low (Kronberg 1994; R. Durrer Département de Physique Théorique and Center for Astroparticle Physics, Université de Genève 24…”
• THE EVOLUTION OF CATACLYSMIC VARIABLES AS REVEALED BY THEIR DONOR STARS (2011, background): “…evidence from noninteracting low-mass stars that fully convective objects (and perhaps even brown dwarfs) can sustain significant magnetic field (e.g., Reiners 2009; Basri 2009; Donati & Landstreet 2009) and experience at least some spin-down due to MB (e.g., Barnes 2003; Reiners & Basri 2008).”
• The MiMeS survey of Magnetism in Massive Stars : magnetic analysis of the O-type stars (2016, background): “…that main sequence and premain sequence magnetic A and B stars generally rotate at a fraction of the speed of non-magnetic A and B stars (e.g. Donati & Landstreet 2009; Alecian et al. 2013), likely as a result of the shedding of angular momentum due to magnetic coupling to the stellar wind…”