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| Query : 2023A&A...680A..12R |
2023A&A...680A..12R - Astronomy and Astrophysics, volume 680A12 (2023/12-1)
Extended far-UV emission surrounding asymptotic giant branch stars as seen by GALEX.
RASTAU V., MECINA M., KERSCHBAUM F., OLOFSSON H., MAERCKER M., DRECHSLER M., STROTTNER X. and MULATO L.
Abstract (from CDS):
Aims. Our goal is to study the long-term mass-loss rate characteristics of asymptotic giant branch (AGB) stars through wind-wind and wind-interstellar medium interaction.
Methods. Far-ultraviolet (FUV) images from the GALEX survey are used to investigate extended UV emission associated with AGB stars.
Results. FUV emission was found towards eight objects. The emission displays different shapes and sizes; interaction regions were identified, often with infrared counterparts, but no equivalent near-ultraviolet (NUV) emission was found in most cases.
Conclusions. The FUV emission is likely attributed to shock-excited molecular hydrogen, considering the lack of NUV emission and the large space velocities of the objects, and makes it possible to trace old structures that are too faint to be observed, for instance, in the infrared.
Methods. Far-ultraviolet (FUV) images from the GALEX survey are used to investigate extended UV emission associated with AGB stars.
Results. FUV emission was found towards eight objects. The emission displays different shapes and sizes; interaction regions were identified, often with infrared counterparts, but no equivalent near-ultraviolet (NUV) emission was found in most cases.
Conclusions. The FUV emission is likely attributed to shock-excited molecular hydrogen, considering the lack of NUV emission and the large space velocities of the objects, and makes it possible to trace old structures that are too faint to be observed, for instance, in the infrared.
Abstract Copyright: © The Authors 2023
Journal keyword(s): stars: AGB and post-AGB - stars: mass-loss - stars: winds, outflows - ultraviolet: stars
Simbad objects: 13
| Number of rows : 13 |
| N | Identifier | Otype |
ICRS (J2000) RA |
ICRS (J2000) DEC |
Mag U | Mag B | Mag V | Mag R | Mag I | Sp type |
#ref
1850 - 2026 |
#notes |
|---|---|---|---|---|---|---|---|---|---|---|---|---|
| 1 | * 47 Psc | LP* | 00 28 02.9147612952 | +17 53 35.257375248 | 8.53 | 6.71 | 5.06 | 3.32 | 1.78 | M3III | 111 | 0 |
| 2 | V* R Scl | C* | 01 26 58.0939182720 | -32 32 35.439234828 | 17.26 | 9.59 | 5.72 | 3.69 | 2.30 | C-N5+ | 354 | 0 |
| 3 | * omi Cet | Mi* | 02 19 20.79210 | -02 58 39.4956 | 7.63 | 6.53 | 5.03 | M5-9IIIe+DA | 1586 | 0 | ||
| 4 | V* R Dor | AB* | 04 36 45.59127 | -62 04 37.7974 | 7.84 | 6.98 | 5.40 | 2.71 | -0.44 | M8III:e | 376 | 0 |
| 5 | IRC +10216 | C* | 09 47 57.40632 | +13 16 43.5648 | C9,5e | 2455 | 0 | |||||
| 6 | V* RW LMi | C* | 10 16 02.2777043904 | +30 34 19.045098516 | 15.27 | C4,3e | 411 | 0 | ||||
| 7 | V* U Ant | C* | 10 35 12.8510147472 | -39 33 45.324020448 | 15.32 | 8.22 | 5.38 | 3.18 | 1.86 | C-N3 | 162 | 0 |
| 8 | V* W Hya | Mi* | 13 49 02.0018313132 | -28 22 03.532006894 | 8.97 | 7.70 | M7.5-9e | 672 | 0 | |||
| 9 | HD 120305 | PM* | 13 49 06.9444125304 | -28 22 23.681992368 | 10.13 | 9.52 | F8/G0V | 6 | 0 | |||
| 10 | V* RZ Sgr | S* | 20 15 28.4023889376 | -44 24 37.478466072 | 10.550 | 9.533 | 7.858 | S4,4ep | 79 | 0 | ||
| 11 | V* V420 Vul | Mi* | 20 59 36.8311700208 | +26 28 34.421511324 | 11.0 | 10.81 | N:e: | 18 | 0 | |||
| 12 | * bet Gru | LP? | 22 42 40.05027 | -46 53 04.4752 | 5.33 | 3.73 | 2.11 | 0.20 | -1.57 | M4.5III | 209 | 1 |
| 13 | V* DM Tuc | AB* | 22 57 05.8561963680 | -57 24 04.224759300 | 8.65 | 7.43 | M8III | 34 | 0 |
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