Atmospheric velocity fields in tepid main sequence stars

J. D. Landstreet; F. Kupka; H. A. Ford; T. Officer; T. A. A. Sigut; J. Silaj; S. Strasser; A. Townshend

doi:10.1051/0004-6361/200912083

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Volume 503 / No 3 (September I 2009)

A&A, 503 3 (2009) 973-984

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Table 2:

Main sequence A-type stars in which evidence of velocity fields is directly detected in line profiles.
HD	other	spectral	binarity	$\ensuremath {T_{{\rm e}}}$	$\xi$	depressed	line shape	$\ensuremath{v_{\rm e} \sin i}$
		type				blue wing	discrepancy	weak lines	strong lines
				(K)	( $\ensuremath{{\rm km~s}^{-1}}$ )			( $\ensuremath{{\rm km~s}^{-1}}$ )	( $\ensuremath{{\rm km~s}^{-1}}$ )
2421 A	HR 104 A	A2Vs	SB2	10 000	1.0	weak	none	3.5	3.5
72660	HR 3383	A1V		9650	2.3	weak	weak	5.0	6.1
114330	$\theta$ Vir	A1Vs	VB2	9250	1.3	weak	weak	4.0	5.5
157486 A	HR 6470 A	A0V	SB2	9150	1.9	weak	weak	1.5	3.5
27962	68 Tau	A2IV m	SB1	8975	2.0	weak	weak	11	11.5
103578 A	95 Leo A	A3V	SB2	8300	2.0	strong	strong	3	9
107168	8 Com	A8 m		8150	3.0	weak	weak	13	14
108642 A	HR 4750 A	A2 m	SB1	8100	4.0	strong	strong	2	10
209625	32 Aqr	A5 m	SB1	7700	4.0	strong	strong	4.5	10

Source LaTeX | All tables | In the text

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