Line-profile variations due to adiabatic non-radial pulsations in rotating stars. I. Observable characteristics of spheroidal modes
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Cites background or methods from "Line-profile variations due to adia..."
...A particularly illustrative study in this respect is the one by Schrijvers et al. (1997), where the predicted variability of line-profiles due to adiabatic non-radial pulsations in rotating stars is shown for a large variety of oscillation and rotation parameters....
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...…(1) where 〈3 n 〉 = ∫ ∞ −∞ (3 − 〈3〉)n(1− F(3))d3 ∫ ∞ −∞ (1− F(3))d3 for n = 2, 3 (2) are the second and third normalized central moments of a spectral line denoted as (3, F(3)), adopting the definition used in Schrijvers et al. (1997), and 〈3〉 = ∫ ∞ −∞ 3 (1− F(3))d3 ∫ ∞ −∞ (1− F(3))d3 ....
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...An interesting work in this respect is the one by Schrijvers et al. (1997), where line-profile asymmetry due to a long lifetime oscillation mode of degreeℓ and azimuthal order m in rotating stars is shown for a large variety of oscillation and rotational parameters (the latter quantified in t rms…...
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...We refer the reader to the works by Schrijvers et al. (1997) Article number, page 8 of 17 and Telting & Schrijvers (1997) for a comprehensive illustration of predicted line-profile variations originated by adiabatic non-radial pulsations in rotating stars....
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...The velocity moments of the line-profile (Balona 1986; Aerts et al. 1992; Schrijvers et al. 1997) have been proven to be powerful tools to characterize the temporal behavior of line asymmetry independently of the physical cause that is originating it....
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Additional excerpts
...9), we can derive the pulsation degree l (see Schrijvers et al. 1997)....
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...7), we can confirm that f1 is due to a pulsation mode with l = 0, as the phase shows no significant slope (see Schrijvers et al. 1997)....
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References
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"Line-profile variations due to adia..." refers background in this paper
...Many authors (e.g. Smith 1986; Gies & Kullavanijaya 1988; Kambe & Osaki 1988; Yang et al. 1988; Kambe et al. 1990) have used the number of visible bumps or, equivalently, the blue-to-red phase difference ∆Ψ0 to identify |m| according to ∆Ψ0 = |m|π....
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...In his discussion of the so called k-problem, Smith (1986) mentioned that for high k(0)-values, the toroidal term(s) caused by rotation might be able to mimic the amplitude-distribution characteristics of a low-k(0) mode....
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...The difficulty to derive k-values from amplitude diagrams The determination of the k-value from observed lineprofiles has been discussed by several authors (e.g. Smith 1986; Kambe et al. 1990; Lee & Saio 1990)....
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