High-precision magnetic field measurements of Ap and Bp stars
By G. Wade, J. Donati, J. Landstreet, S. Shorlin. 2000
178 citations recorded by the source corpus.
Subfields: Astronomy and Astrophysics
View Paper: https://www.semanticscholar.org/paper/00bfc312d6a9e7fb9511d31e955c430e8a93e7fb
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In Astronomy and Astrophysics
Citations in the corpus
- Visual and ultraviolet flux variability of the bright CP star θ Aurigae (2015, methodology): “…(1977) 1984 IUE 106 -1207 -0.05(10) this paper 1992 Hp 131 -398 0.03(3) ESA (1997) 1994 uvby 188 -210 -0.02(2) Adelman (1997) 1998 C 11 209 -0.07(4) Wade et al. (2000) 2004 uvby 276 859 -0.01(2) Adelman et al. (2005) 2008 Bl 7 1206 0.00(2) Silvester et al. (2012) spot profiles in phases,A jλ are…”
- Large-scale magnetic topologies of late M dwarfs★: Magnetic topologies of late M dwarfs (2010, background): “…Stokes I and V LSD profiles through the relation: Bl(G) = −2.14× 10 11 ∫ v V (v) dv λ0 geff c ∫ [Ic − I(v)] dv , (1) (Rees & Semel 1979; Donati et al. 1997; Wade et al. 2000) where v is the radial velocity in the star’s rest frame, λ0, in nm, is the mean wavelength of the LSD profile, c is the…”
- Large-scale magnetic topologies of late M dwarfs⋆ (2008, background): “…I and V LSD profiles through the relation : Bl(G) = −2.14 × 10 11 Z v V (v) dv λ0 geff c Z [Ic − I(v)] dv , (1) (Rees & Semel 1979; Donati et al. 1997a; Wade et al. 2000) where v is the radial velocity in the star’s rest frame, λ0, in nm, is the mean wavelength of the LSD profile, c is the…”
- Magnetic Fields of Nondegenerate Stars (2009, background): “…of StokesV profiles (as well as StokesQ andU profiles whenever available) of magnetic Ap/B stars collected over full rotational cycles (e.g., Wade et al. 2000) show that these stars also feature a significant amount of medium-scale magnetic structures that are not properly described with…”
- Least-squares deconvolution of the stellar intensity and polarization spectra (2010, methodology): “Wade et al. (2000b) established a similar relation for the scaling of the linear polarization profiles, but they usedg2 instead ofG in the line weightwQ.”
- A high-resolution spectropolarimetric survey of Herbig Ae/Be stars – I. Observations and measurements (2012, result): “…〈Bz〉 is determined by computing the first-order moment of Stokes V, normalized to the equivalent width of Stokes I (Mathys 1991; Donati et al. 1997; Wade et al. 2000): 〈Bz〉 = −2.14 × 1011 ∫ vV (v) dv λḡc ∫ [Ic − I (v)] dv , (1) where 〈Bz〉 is in G, ḡ is the mean Landé factor of the LSD weights…”