X-ray study of bow shocks in runaway stars
Massive runaway stars produce bow shocks through the interaction of their winds with the interstellar medium, with the prospect for particle acceleration by the shocks. These objects are consequently candidates for non-thermal emission. Our aim is to investigate the X-ray emission from these sources...
| Autores principales: | , , , , |
|---|---|
| Formato: | Articulo |
| Lenguaje: | Inglés |
| Publicado: |
2017
|
| Materias: | |
| Acceso en línea: | http://sedici.unlp.edu.ar/handle/10915/125731 |
| Aporte de: |
| id |
I19-R120-10915-125731 |
|---|---|
| record_format |
dspace |
| institution |
Universidad Nacional de La Plata |
| institution_str |
I-19 |
| repository_str |
R-120 |
| collection |
SEDICI (UNLP) |
| language |
Inglés |
| topic |
Astronomía acceleration of particles radiation mechanisms: non-thermal stars: earlytype X-rays: stars |
| spellingShingle |
Astronomía acceleration of particles radiation mechanisms: non-thermal stars: earlytype X-rays: stars De Becker, Michaël Valle, M. V. del Romero, Gustavo Esteban Peri, Cintia Soledad Benaglia, Paula X-ray study of bow shocks in runaway stars |
| topic_facet |
Astronomía acceleration of particles radiation mechanisms: non-thermal stars: earlytype X-rays: stars |
| description |
Massive runaway stars produce bow shocks through the interaction of their winds with the interstellar medium, with the prospect for particle acceleration by the shocks. These objects are consequently candidates for non-thermal emission. Our aim is to investigate the X-ray emission from these sources. We observed with XMM–Newton a sample of five bow shock runaways, which constitutes a significant improvement of the sample of bow shock runaways studied in X-rays so far. A careful analysis of the data did not reveal any X-ray emission related to the bow shocks. However, X-ray emission from the stars is detected, in agreement with the expected thermal emission from stellar winds. On the basis of background measurements we derive conservative upper limits between 0.3 and 10 keV on the bow shocks emission. Using a simple radiation model, these limits together with radio upper limits allow us to constrain some of the main physical quantities involved in the non-thermal emission processes, such as the magnetic field strength and the amount of incident infrared photons. The reasons likely responsible for the non-detection of non-thermal radiation are discussed. Finally, using energy budget arguments, we investigate the detectability of inverse Compton X-rays in a more extended sample of catalogued runaway star bow shocks. From our analysis we conclude that a clear identification of non-thermal X-rays from massive runaway bow shocks requires one order of magnitude (or higher) sensitivity improvement with respect to present observatories. |
| format |
Articulo Articulo |
| author |
De Becker, Michaël Valle, M. V. del Romero, Gustavo Esteban Peri, Cintia Soledad Benaglia, Paula |
| author_facet |
De Becker, Michaël Valle, M. V. del Romero, Gustavo Esteban Peri, Cintia Soledad Benaglia, Paula |
| author_sort |
De Becker, Michaël |
| title |
X-ray study of bow shocks in runaway stars |
| title_short |
X-ray study of bow shocks in runaway stars |
| title_full |
X-ray study of bow shocks in runaway stars |
| title_fullStr |
X-ray study of bow shocks in runaway stars |
| title_full_unstemmed |
X-ray study of bow shocks in runaway stars |
| title_sort |
x-ray study of bow shocks in runaway stars |
| publishDate |
2017 |
| url |
http://sedici.unlp.edu.ar/handle/10915/125731 |
| work_keys_str_mv |
AT debeckermichael xraystudyofbowshocksinrunawaystars AT vallemvdel xraystudyofbowshocksinrunawaystars AT romerogustavoesteban xraystudyofbowshocksinrunawaystars AT pericintiasoledad xraystudyofbowshocksinrunawaystars AT benagliapaula xraystudyofbowshocksinrunawaystars |
| bdutipo_str |
Repositorios |
| _version_ |
1764820452136452097 |