2010A&A...512A..73M


C.D.S. - SIMBAD4 rel 1.7 - 2020.02.18CET07:31:55

2010A&A...512A..73M - Astronomy and Astrophysics, volume 512, A73-73 (2010/3-1)

Resolving the dusty circumstellar environment of the A[e] supergiant HD 62623 with the VLTI/MIDI.

MEILLAND A., KANAAN S., BORGES FERNANDES M., CHESNEAU O., MILLOUR F., STEE P. and LOPEZ B.

Abstract (from CDS):

B[e] stars are hot stars surrounded by circumstellar gas and dust which is responsible for the presence of emission lines and IR-excess in their spectra. How dust can be formed in this highly illuminated and diluted environment remains an open issue. HD 62623 is one of the very few A-type supergiants showing the B[e] phenomenon. We studied the geometry of its circumstellar envelope in the mid-infrared using long-baseline interferometry, which is the only observing technique able to spatially resolve objects smaller than a few tens of milliarcseconds. We obtained nine calibrated visibility measurements between October 2006 and January 2008 using the VLTI/MIDI instrument in SCI-PHOT mode and PRISM spectral dispersion mode with projected baselines ranging from 13 to 71m and with various position angles (PA). We used geometrical models and physical modeling with a radiative transfer code to analyze these data. The dusty circumstellar environment of HD 62623 is partially resolved by the VLTI/MIDI, even with the shortest baselines. The environment is flattened (a/b∼1.3±0.1) and can be separated into two components: a compact one whose extension grows from 17mas at 8µm to 30mas at 9.6µm and stays almost constant up to 13µm, and a more extended one that is over-resolved even with the shortest baselines. Using the radiative transfer code MC3D, we managed to model HD 62623's circumstellar environment as a dusty disk with an inner radius of 3.85±0.6AU, an inclination angle of 60±10°, and a mass of 2x10–7M. It is the first time that the dusty disk inner rim of a supergiant star exhibiting the B[e] phenomenon is significantly constrained. The inner gaseous envelope likely contributes up to 20% to the total N band flux and acts like a reprocessing disk. Finally, the hypothesis of a stellar wind deceleration by the companion's gravitational effects remains the most probable case since the bi-stability mechanism does not seem to be efficient for this star.

Abstract Copyright:

Journal keyword(s): techniques: high angular resolution - techniques: interferometric - stars: emission-line, Be - stars: winds, outflows - stars: individual: HD 62623 - circumstellar matter

Simbad objects: 14

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Number of rows : 14

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 * alf Eri Be* 01 37 42.84548 -57 14 12.3101 -0.36 0.30 0.46 0.49 0.60 B6Vpe 442 0
2 * 4 Eri PM* 02 57 23.7661415506 -23 51 43.792006336   5.68 5.45     A5IV/V 39 0
3 * gam Eri LP? 03 58 01.7669489 -13 30 30.669770 6.52 4.54 2.94 1.68 0.68 M0III-IIIb 168 0
4 * alf CMa SB* 06 45 08.91728 -16 42 58.0171 -1.51 -1.46 -1.46 -1.46 -1.43 A1V+DA 1383 0
5 * kap CMa Be* 06 49 50.4593263 -32 30 30.522482 2.73 3.68 3.89 3.91 4.05 B1.5Ve 270 0
6 * alf CMi SB* 07 39 18.11950 +05 13 29.9552 0.82 0.79 0.37 -0.05 -0.28 F5IV-V+DQZ 1748 0
7 * l Pup sg* 07 43 48.4687222 -28 57 17.372015 4.06 4.09 3.93 3.68 3.50 A4Iabe 174 0
8 * alf Hya * 09 27 35.24270 -08 39 30.9583 5.14 3.42 1.97 0.93 0.16 K3IIIa 404 0
9 HD 87643 Em* 10 04 30.2845136666 -58 39 52.138769673 8.92 10.38 9.50 9.68   B3I[e] 133 0
10 CD-57 3107 Em* 10 15 21.9719703212 -57 51 42.737312199 12.27 11.72 10.15 9.78   M3 36 0
11 * del Sco SB* 16 00 20.00528 -22 37 18.1431 1.30 2.20 2.32 2.36 2.49 B0.3IV 688 0
12 * alf Ara Be* 17 31 50.4915282 -49 52 34.122041 2.09 2.78 2.95 3.05 3.29 B2Vne 243 0
13 * alf Cyg sg* 20 41 25.91514 +45 16 49.2197 1.11 1.34 1.25 1.14 1.04 A2Ia 714 0
14 * bet Gru LP? 22 42 40.05027 -46 53 04.4752 5.33 3.73 2.11 0.20 -1.57 M4.5III 192 0

    Equat.    Gal    SGal    Ecl

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2020.02.18-07:31:55

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