2011A&A...529A..34M


C.D.S. - SIMBAD4 rel 1.7 - 2019.10.22CEST04:20:38

2011A&A...529A..34M - Astronomy and Astrophysics, volume 529A, 34-34 (2011/5-1)

Optical spectroscopic variability of Herbig Ae/Be stars.

MENDIGUTIA I., EIROA C., MONTESINOS B., MORA A., OUDMAIJER R.D., MERIN B. and MEEUS G.

Abstract (from CDS):

In order to gain insights into the variability behaviour of the circumstellar (CS) atomic gas, we have analysed 337 multi-epoch optical spectra of 38 Herbig Ae/Be (HAeBe) stars. Equivalent widths (EWs) and line fluxes of the Hα, [OI]6300, HeI5876 and NaID lines were obtained for each spectrum; the Hα line width at 10% of peak intensity (W10) and profile shapes were also measured and classified. The mean line strengths and relative variabilities were quantified for each star. Simultaneous optical photometry was used to estimate the line fluxes. We present a homogeneous spectroscopic database of HAeBe stars. The lines are variable in practically all stars and timescales, although 30% of the objects show a constant EW in [OI]6300, which is also the only line that shows no variability on timescales of hours. The HeI5876 and NaID EW relative variabilities are typically the largest, followed by those in [OI]6300 and Hα. The EW changes can be larger than one order of magnitude for the HeI5876 line, and up to a factor 4 for Hα. The [OI]6300 and Hα EW relative variabilities are correlated for most stars in the sample. The Hα mean EW and W10 are uncorrelated, as are their relative variabilities. The Hα profile changes in ∼70% of the objects. The massive stars in the sample (M *>3M ) usually show more stable Hα profiles with blueshifted self-absorptions and less variable 10% widths. Our data suggest multiple causes for the different line variations, but the [OI]6300 and Hα variability must share a similar origin in many objects. The physical mechanism responsible for the Hα line broadening does not depend on the amount of emission; unlike in lower-mass stars, physical properties based on the Hα luminosity and W10 would significantly differ. Our results provide additional support to previous works that reported different physical mechanisms in Herbig Ae and Herbig Be stars. The multi-epoch observations we present are a useful tool for understanding the origin of the CS lines and their variability, and to establish distinctions in the physical processes operating in pre-main sequence stars.

Abstract Copyright:

Journal keyword(s): stars: pre-main sequence - stars: activity - circumstellar matter - accretion, accretion disks - protoplanetary disks

Simbad objects: 38

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Number of rows : 38

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2019
#notes
1 V* VX Cas Ae* 00 31 30.6816836826 +61 58 50.982831889 11.83 11.59 10.50 11.19 10.94 A0Vep 125 0
2 V* XY Per Ae* 03 49 36.32389 +38 58 55.6050 12.12 9.47 9.80 8.70 8.40 A2II+B6 140 0
3 V* RY Tau TT* 04 21 57.4132838427 +28 26 35.533990877 10.82 10.34 9.30 9.67 8.87 K1IV/Ve 633 1
4 HD 31648 Ae* 04 58 46.2654165113 +29 50 36.990341242 7.84 7.78 7.62 7.76 7.43 A5Vep 372 0
5 V* UX Ori Ae* 05 04 29.9881676817 -03 47 14.288047238 10.25 10.93 8.70 9.62 9.43 A4IVe 327 1
6 V* V1366 Ori EB* 05 16 00.4764811920 -09 48 35.394685295 10.19 10.16 9.84 9.77 9.63 B9.5V 158 0
7 HD 34700 TT* 05 19 41.4088548858 +05 38 42.777125431 9.75 9.788 9.15 8.80 8.47 G0IVe 65 2
8 HD 287841 Y*O 05 24 42.8031051407 +01 43 48.249517233 10.55 10.45 10.17 9.99 9.80 A8V 83 0
9 V* CO Ori TT* 05 27 38.3352 +11 25 38.923 12.96 12.33 10.30 10.33 9.63 F7Ve 155 0
10 V* HK Ori Ae* 05 31 28.0451235474 +12 09 10.149849783 11.82 12.06 11.10 11.02 10.56 A2?e+G0?e 173 1
11 V* RY Ori Or* 05 32 09.9419985443 -02 49 46.769539985 12.62 12.76 10.80 10.82 10.34 F7 45 0
12 V* NV Ori Ae* 05 35 31.3684708885 -05 33 08.871090196 10.36 10.21 8.70 9.48 9.22 F6IIIe 84 0
13 V* T Ori Ae* 05 35 50.4483740019 -05 28 34.923375739 12.724 11.637 11.248 10.09 10.043 A3IVeb 226 0
14 V* CQ Tau Ae* 05 35 58.4671238887 +24 44 54.086375712 11.290 10.780 10.000   8.33 F5IVe 245 0
15 V* BF Ori Ae* 05 37 13.2623698298 -06 35 00.565420577 10.37 10.00 9.69 10.06 9.31 A7III 266 0
16 V* RR Tau Ae* 05 39 30.5114685049 +26 22 26.961204895 11.64 12.09 11.28 10.58 10.17 A0:IVe 215 0
17 V* V350 Ori Em* 05 40 11.7641189614 -09 42 11.085315699 12.74 12.08 11.42 11.38 10.96 A7V 61 0
18 V* VY Mon Ae* 06 31 06.9180562526 +10 26 04.982093681 16.65 15.45 13.70 12.49 11.00 A5:Vep 85 0
19 V* R Mon Ae* 06 39 09.9538710861 +08 44 09.559404231 10.76 12.46 11.85 10.96 10.25 B8IIIe 498 0
20 HD 58647 Em* 07 25 56.0988044433 -14 10 43.548997982 6.81 6.92 6.85 6.73 6.73 B9IV 69 0
21 HD 141569 pr* 15 49 57.7484743862 -03 55 16.344023102 7.22 7.20 7.12 7.00 7.04 A2VekB9mB9(_lB) 454 0
22 HD 142666 TT* 15 56 40.0222941557 -22 01 40.004849949 9.41 9.37 8.82 8.31 8.01 F0V_sh 202 0
23 HD 144432 Ae* 16 06 57.9530266912 -27 43 09.758016578 8.47 8.53 8.19 7.82 7.53 A9/F0V 206 1
24 HD 150193 Be* 16 40 17.9242900066 -23 53 45.192676418 9.69 9.32 8.79 8.41   B9.5Ve 284 0
25 EM* AS 220 Ae* 17 10 08.1238 -27 15 18.801 12.86 12.79 12.22 12.03 10.82 A6Ve+G5Ve 125 0
26 * c Oph Be* 17 31 24.9541340 -23 57 45.513592 4.75 4.81 4.81 4.74 4.72 A0V 250 0
27 HD 163296 Ae* 17 56 21.2882188601 -21 57 21.872343282 7.00 6.93 6.85 6.86 6.67 A1Vep 729 0
28 V* VV Ser Ae* 18 28 47.8619658319 +00 08 39.924642619 12.99 12.63 11.80 11.01 10.24 A5Ve 224 0
29 HD 179218 Ae* 19 11 11.2540715594 +15 47 15.632212730 7.55 7.476 7.39 7.25 7.21 A0Ve 213 0
30 V* WW Vul Ae* 19 25 58.7494596284 +21 12 31.333220807 11.46 10.99 10.25 10.38 10.12 A2IVe 214 0
31 V* PX Vul Or* 19 26 40.2533631097 +23 53 50.777553057 12.56 12.57 11.83 10.90 10.30 F3Ve 49 0
32 HD 190073 Ae* 20 03 02.5098091524 +05 44 16.658081203 7.91 7.86 7.73   7.65 A2IVe 219 0
33 EM* LkHA 224 Ae* 20 20 29.3500765489 +41 21 28.448014439 14.82 14.08 12.93 12.05 11.08 A4:Ve 90 0
34 EM* AS 442 Ae* 20 47 37.4658048789 +43 47 24.973275249 11.90 11.56 10.90 10.18 9.95 B8Ve 81 0
35 EM* LkHA 234 Ae* 21 43 06.823 +66 06 54.24 13.65 13.61 12.73 11.98 11.20 B5Ve 272 0
36 V* BH Cep Ae* 22 01 42.8726806026 +69 44 36.423728031 12.18 11.54 11.01 10.62 10.32 F5IIIe 53 0
37 V* BO Cep Ae* 22 16 54.0590233441 +70 03 44.984949208 11.86 11.98 11.55 11.16 10.84 F5Ve 60 0
38 V* SV Cep Ae* 22 21 33.2175224577 +73 40 27.096415978 11.40 11.25 10.35 10.28 10.08 A2IVe 122 0

    Equat.    Gal    SGal    Ecl

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2019.10.22-04:20:38

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