2018A&A...614A...3R


Query : 2018A&A...614A...3R

2018A&A...614A...3R - Astronomy and Astrophysics, volume 614A, 3-3 (2018/6-1)

The co-existence of hot and cold gas in debris discs.

REBOLLIDO I., EIROA C., MONTESINOS B., MALDONADO J., VILLAVER E., ABSIL O., BAYO A., CANOVAS H., CARMONA A., CHEN C., ERTEL S., GARUFI A., HENNING T., IGLESIAS D.P., LAUNHARDT R., LISEAU R., MEEUS G., MOOR A., MORA A., OLOFSSON J., RAUW G. and RIVIERE-MARICHALAR P.

Abstract (from CDS):


Context. Debris discs have often been described as gas-poor discs as the gas-to-dust ratio is expected to be considerably lower than in primordial, protoplanetary discs. However, recent observations have confirmed the presence of a non-negligible amount of cold gas in the circumstellar (CS) debris discs around young main-sequence stars. This cold gas has been suggested to be related to the outgassing of planetesimals and cometary-like objects.
Aims. The goal of this paper is to investigate the presence of hot gas in the immediate surroundings of the cold-gas-bearing debris-disc central stars.
Methods. High-resolution optical spectra of all currently known cold-gas-bearing debris-disc systems, with the exception of β Pic and Fomalhaut, have been obtained from La Palma (Spain), La Silla (Chile), and La Luz (Mexico) observatories. To verify the presence of hot gas around the sample of stars, we have analysed the CaII H&K and the NaI D lines searching for non-photospheric absorptions of CS origin, usually attributed to cometary-like activity.
Results. Narrow, stable CaII and/or NaI absorption features have been detected superimposed to the photospheric lines in 10 out of the 15 observed cold-gas-bearing debris-disc stars. Features are found at the radial velocity of the stars, or slightly blue- or red-shifted, and/or at the velocity of the local interstellar medium (ISM). Some stars also present transient variable events or absorptions extended towards red wavelengths (red wings). These are the first detections of such CaII features in 7 out of the 15 observed stars. Although anISM origin cannot categorically be excluded, the results suggest that the stable and variable absorptions arise from relatively hot gas located in the CS close-in environment of the stars. This hot gas is detected in at least ∼80%, of edge-on cold-gas-bearing debris discs, while in only ∼10% of the discs seen close to face-on. We interpret this result as a geometrical effect, and suggest that the non-detection of hot gas absorptions in some face-on systems is due to the disc inclination and likely not to the absence of the hot-gas component. This gas is likely released in physical processes related in some way to the evaporation of exocomets, evaporation of dust grains, or grain-grain collisions close to the central star.

Abstract Copyright: © ESO 2018

Journal keyword(s): stars: general - planetary systems - comets: general - ISM: clouds - circumstellar matter

VizieR on-line data: <Available at CDS (J/A+A/614/A3): list.dat sp/*>

Errata: erratum vol. 625, art. C2 (2019)

Status at CDS : Objects in title, abstract, text, figures, and all or part of small table(s) being processed in SIMBAD.

Simbad objects: 40

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Number of rows : 40
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 * 49 Cet PM* 01 34 37.7788265080 -15 40 34.898112472   5.667 5.607   5.54 A1V 258 0
2 HD 21997 PM* 03 31 53.6468412720 -25 36 50.936416301   6.501 6.372   6.25 A3IV/V 136 0
3 HD 32297 * 05 02 27.4357771761 +07 27 39.682335894   8.32 8.14     A0V 160 0
4 * bet Pic PM* 05 47 17.0876901 -51 03 59.441135 4.13 4.03 3.86 3.74 3.58 A6V 1729 1
5 * eta Crv PM* 12 32 04.2265302 -16 11 45.616473   4.658 4.294     F2V 292 0
6 HD 110058 * 12 39 46.1959400684 -49 11 55.552264268   8.12 7.97     A0V 63 0
7 HD 121191 * 13 55 18.8788456136 -53 31 42.713405012   8.40 8.16     A5IV/V 26 0
8 HD 121617 * 13 57 41.1259337352 -47 00 34.249785107   7.36 7.29     A1V 35 0
9 HD 128207 * 14 36 44.1324736454 -40 12 41.689720406   5.624 5.736     B8V 48 0
10 HR 5543 ** 14 52 51.0737484 -37 48 11.386959 4.11 4.855 5.015     B7IIIp 114 0
11 HD 131488 * 14 55 08.0285082411 -41 07 13.401062817   8.09 8.00     A1V 23 0
12 HD 131835 * 14 56 54.4676957121 -35 41 43.659216390   8.05 7.86     A2IV 94 0
13 HD 132094 * 14 58 24.2647270652 -37 21 44.898238966   7.25 7.25     B9V 28 0
14 * bet Lup PM* 14 58 31.92536 -43 08 02.2699 1.59 2.46 2.68 2.78 2.95 B2III 180 0
15 * kap Cen ** 14 59 09.6849382 -42 06 15.106919 2.15 2.93 3.11     B2IV 193 0
16 HD 132955 * 15 02 59.2752145072 -32 38 35.855774022 4.69 5.319 5.437     B3V 87 0
17 V* HR Lup a2* 15 08 12.1245697358 -40 35 02.158712447 5.25 5.65 5.79     B8IVSi 157 1
18 HD 133937 * 15 08 39.1976637682 -42 52 04.518555417   5.701 5.820     B5/7V 70 0
19 HD 135454 * 15 16 37.1492904047 -42 22 12.564257632   6.716 6.754     B9.5V 32 0
20 HD 136246 * 15 20 31.4189361841 -28 17 13.583790033   7.26 7.16     A1V 35 0
21 HD 138813 * 15 35 16.1057045661 -25 44 02.991140952   7.37 7.30     A0V 67 0
22 * b Sco * 15 50 58.7451174285 -25 45 04.662754169 3.84 4.552 4.635     B1.5Vn 274 0
23 HD 142184 Be* 15 53 55.86404 -23 58 41.1522 4.77 5.352 5.402     B2V 206 0
24 HD 142250 * 15 54 30.1091550054 -27 20 19.084473313   6.07 6.10     B7V 101 0
25 * 3 Sco Ro* 15 54 39.5292926476 -25 14 37.459112692 5.23 5.81 5.87     B8III/IV 197 0
26 HD 144587 * 16 07 29.9254002047 -23 57 02.451154978   8.73 8.31     A9V 47 0
27 HD 145554 * 16 12 21.8333006041 -19 34 44.570507060   7.77 7.64     B9V 79 0
28 HD 145631 * 16 12 44.1005300475 -19 30 10.346758641   7.73 7.60     B9V 83 0
29 HD 145964 * 16 14 28.8830612483 -21 06 27.490846733   6.407 6.405     B9V 74 0
30 HD 146897 Ro* 16 19 29.2420604682 -21 24 13.271535164   9.58 9.11     F2/3V 71 0
31 HD 147137 dS* 16 20 50.2316342158 -22 35 38.790860826   9.42 9.03   8.44 A9V 55 0
32 HD 147932 Ro* 16 25 35.0836168833 -23 24 18.788751256 7.24 7.59 7.27     B5V 112 0
33 HD 156623 * 17 20 50.6168249548 -45 25 14.996684006   7.35 7.26     A0V 52 0
34 HD 172555 PM* 18 45 26.9004853 -64 52 16.539796   4.967 4.767     A7V 247 0
35 * eta Tel PM* 19 22 51.2064652963 -54 25 26.152538950   5.035 5.020   4.99 A0V+M7/8V 196 0
36 TYC 3134-1024-1 * 19 22 52.9409787488 +38 41 41.487237394   10.41 9.98     ~ 11 0
37 HD 181327 PM* 19 22 58.9434412361 -54 32 16.979671096   7.50 7.04   6.49 F6V 244 0
38 HD 181298 * 19 25 22.6537211254 -68 42 59.855044016   10.385 9.77 9.44 9.199 F8/G0(V) 9 0
39 BD+48 2901 * 19 28 41.1976399160 +48 41 15.133338838   10.38 10.03     F5V 10 0
40 * alf PsA ** 22 57 39.04625 -29 37 20.0533 1.31 1.25 1.16 1.11 1.09 A4V 1154 3

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2021.09.23-05:00:19

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