Searching for a link between the magnetic nature and other observed properties of Herbig Ae/Be stars and stars with debris disks

Home

All issues

Volume 502 / No 1 (July IV 2009)

A&A, 502 1 (2009) 283-301

Full HTML

Free Access

Table 7:

Rotation periods of stars with known inclinations.
Object	Inclination	Adopted	v sin i	$v_{\rm eq}$	R	P
name	Measurements	Inclination	[km s^-1]	[km s^-1]	[ $R_{\odot}$ ]	[d]
	[ $^\circ$ ]	[ $^\circ$ ]
HD 95881	40-55¹	40-55	50^q	61-78	3.1^dd	2.0-2.6
HD 97048	30-40^a	30-40	140^r	218-280	2.5^ee	0.5-0.6
	42.8^b
HD 100453	>55²	>55	39^s	<48	1.7^ff	>1.8
HD 100546	42^c	$47\pm5$	65^t	82-97	1.7^ff	0.9-1.0
	51^d
HD 101412	>55³	>55	5^u	<6.1	2.1^gg	>17.4
HD 135344B	11^e	11	69^v	362	2.4^gg	0.3
	14^f
HD 139614	<40^g	<40	15^w	>23	1.6^dd	<3.5
HD 144432	48 $\pm$ 10^e	48 $\pm$ 10	70^w	83-114	3.0^ff	1.3-1.8
HD 144668	58^h	58	100^w	118	3.9^ee	1.7
HD 150193	$\sim$ 38ⁱ	30⁵	100^t	200	2.1^ee	0.5
HD 152404	65-70^j	65-70	$18.5\pm1$ ^j	18.5-21.5	2.6^dd	6.1-7.1
HD 158643	$\sim$ 90^k	90	$267\pm5$ ^v	267 $\pm$ 5	5.3^hh	1.0
			228^x	228
HD 163296	51 ^+11,_-9^l	51	130^w	167	2.8^ee	0.8
HD 169142	13 $\pm$ 2^e	$13\pm2$	$66\pm2$ ^v	247-356	1.6^dd	0.2-0.3
VV Ser	72 $\pm$ 5^f	72	142^y	149	2.4^ee	0.8
			229^z	241
HD 179218	$40\pm10$ ^e	$40\pm10$	60^aa	78-120	4.8^gg	2.0-3.1
HD 190073	<40⁴	<40	12^bb	>18.7	3.3^ff	<8.9
HD 9672	90^m	90	196^x	196	1.7ⁱⁱ	0.4
HD 39060	87ⁿ	87	130^k	130	1.8^jj	0.7
HD 109573	73^o	73	152^x	159	1.8^gg	0.6
HD 181327	31.7^p	31.7	16^cc	30	1.2^gg	2.0

Notes: Inclination angles derived for resolved disk detections from the literature and from the study of Mg II spectral line profiles in UV spectra or the study of H $\alpha$ line profiles in optical spectra and the inclination values we finally adopt for further use are listed in Cols. 2 and 3. v sin i values and radii presented in Cols. 4 and 6, respectively, are for the most part gathered from the literature. In Col. 7 we present the equatorial velocity values which are obtained from the inclination angles and the v sin i values. $v_{\rm eq}$ and radii are used to estimate the rotation periods listed in the last column. Radii marked as this study were calculated using $T_{\rm eff}$ and bolometric luminosity, both taken from the literature.
References: ^a Doering et al. (2007), ^b Doucet et al. (2007), ^c Ardila et al. (2007), ^d Augereau et al. (2001), ^e Dent et al. (2005), ^f Pontoppidan et al. (2008), ^g Meeus et al. 1998, ^h Preibisch et al. (2006), ⁱ Fukagawa et al. (2003), ^j Alencar et al. (2003), ^k Slettebak (1982), ^l Wassell et al. (2006), ^m Hughes et al. (2008), ⁿ Heap et al. (2000), ^o Schneider et al. (1999), ^p Schneider et al. (2006), ^q Grady et al. (1996), ^r van den Ancker (1998), ^s Acke & Waelkens (2004), ^t Hamidouche et al. (2008), ^u this study (see Sect. 4.1), ^v Dunkin et al. (1997), ^w Hubrig et al. (2007b), ^x Royer et al. (2007), ^y Vieira et al. (2003), ^z Mora et al. (2001), ^aa Bernacca & Perinotto (1970), ^bb Pogodin et al. (2005), ^cc de la Reza & Pinzón (2004), ^dd Blondel & Tjin (2006), ^ee Hillenbrand et al. (1992), ^ff Wade et al. (2007), ^gg this study (see table caption), ^hh Tatulli et al. (2008), ⁱⁱ Hughes et al. (2008), and ^jj di Folco et al. (2004).
Comments on the inclination angles deduced in this study, mainly from IUE (LWR and LWP cameras) through analysis of line profile types. Profile shapes are classified according to Beals (1951). See also the discussion in Sect. 4.1. ¹ Mg II alternates between P Cygni type I (red emission, with blue-shifted absorption, IUE LWP 30 772) and type III (double emission, IUE LWP 13 082), ² the H $\alpha$ profile shown by Meeus et al. (2002) shows characteristic double-peaked H $\alpha$ emission, ³ see the discussion in Sect. 4.1, ⁴ Mg II has a type I P Cygni profile (IUE LWP 25 762, LWR 11 977, LWR 08 996), ⁵ Mg II has a type I profile (IUE LWP 13 083).

Source LaTeX | All tables | In the text

Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.

Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.

Initial download of the metrics may take a while.