Winds of Wolf−Rayet stars: phenomenology of mass loss
Population I Wolf–Rayet (WR) stars are the evolved descendants of massive (M ≥ 25M) O-type stars. The dense, fast radiatively-drivenWR winds efficiently hide all vital information about basic characteristics of the stellar cores. Observing binary systems with WR components, we put firm limits on the...
Gespeichert in:
| Veröffentlicht in: | Кинематика и физика небесных тел |
|---|---|
| Datum: | 2005 |
| 1. Verfasser: | |
| Format: | Artikel |
| Sprache: | Englisch |
| Veröffentlicht: |
Головна астрономічна обсерваторія НАН України
2005
|
| Schlagworte: | |
| Online Zugang: | https://nasplib.isofts.kiev.ua/handle/123456789/79404 |
| Tags: |
Tag hinzufügen
Keine Tags, Fügen Sie den ersten Tag hinzu!
|
| Назва журналу: | Digital Library of Periodicals of National Academy of Sciences of Ukraine |
| Zitieren: | Winds of Wolf−Rayet stars: phenomenology of mass loss / S.V. Marchenko // Кинематика и физика небесных тел. — 2005. — Т. 21, № 5-додаток. — С. 23-29. — Бібліогр.: 54 назв. — англ. |
Institution
Digital Library of Periodicals of National Academy of Sciences of Ukraine| _version_ | 1862738369139703808 |
|---|---|
| author | Marchenko, S.V. |
| author_facet | Marchenko, S.V. |
| citation_txt | Winds of Wolf−Rayet stars: phenomenology of mass loss / S.V. Marchenko // Кинематика и физика небесных тел. — 2005. — Т. 21, № 5-додаток. — С. 23-29. — Бібліогр.: 54 назв. — англ. |
| collection | DSpace DC |
| container_title | Кинематика и физика небесных тел |
| description | Population I Wolf–Rayet (WR) stars are the evolved descendants of massive (M ≥ 25M) O-type stars. The dense, fast radiatively-drivenWR winds efficiently hide all vital information about basic characteristics of the stellar cores. Observing binary systems with WR components, we put firm limits on the sizes and luminosities ofWR stars. In attempt to understand dynamics of the outflows, we study the micro-structure of WR winds, finding that they are composed from numerous dense clumps. The growing evidence that WR stars may be linked (collapsars) to the long Gamma Ray Bursters raises a question about rotation rates of WR stars. First results based on the observations of globally-structured winds of some WR stars show that they may be considered as moderately fast rotators. There is one more fascinating feature of the WR mass loss: some carbon-reach WR stars may form dust, thus placing them among the first prodigious dust-producers in the early Universe. Though we are yet to find how dust is formed in the extremely hostile environment of WR winds, we have made substantial progress over the past decade. Recent high spatial resolution near/mid-infrared imaging at the HST, Keck and Gemini, combined with abundant optical/UV spectroscopy and photometry, allows to map rapidly changing environments of the dust-forming regions and derive some basic properties of the freshly formed dust.
|
| first_indexed | 2025-12-07T20:03:44Z |
| format | Article |
| fulltext | |
| id | nasplib_isofts_kiev_ua-123456789-79404 |
| institution | Digital Library of Periodicals of National Academy of Sciences of Ukraine |
| issn | 0233-7665 |
| language | English |
| last_indexed | 2025-12-07T20:03:44Z |
| publishDate | 2005 |
| publisher | Головна астрономічна обсерваторія НАН України |
| record_format | dspace |
| spelling | Marchenko, S.V. 2015-03-31T20:15:09Z 2015-03-31T20:15:09Z 2005 Winds of Wolf−Rayet stars: phenomenology of mass loss / S.V. Marchenko // Кинематика и физика небесных тел. — 2005. — Т. 21, № 5-додаток. — С. 23-29. — Бібліогр.: 54 назв. — англ. 0233-7665 https://nasplib.isofts.kiev.ua/handle/123456789/79404 Population I Wolf–Rayet (WR) stars are the evolved descendants of massive (M ≥ 25M) O-type stars. The dense, fast radiatively-drivenWR winds efficiently hide all vital information about basic characteristics of the stellar cores. Observing binary systems with WR components, we put firm limits on the sizes and luminosities ofWR stars. In attempt to understand dynamics of the outflows, we study the micro-structure of WR winds, finding that they are composed from numerous dense clumps. The growing evidence that WR stars may be linked (collapsars) to the long Gamma Ray Bursters raises a question about rotation rates of WR stars. First results based on the observations of globally-structured winds of some WR stars show that they may be considered as moderately fast rotators. There is one more fascinating feature of the WR mass loss: some carbon-reach WR stars may form dust, thus placing them among the first prodigious dust-producers in the early Universe. Though we are yet to find how dust is formed in the extremely hostile environment of WR winds, we have made substantial progress over the past decade. Recent high spatial resolution near/mid-infrared imaging at the HST, Keck and Gemini, combined with abundant optical/UV spectroscopy and photometry, allows to map rapidly changing environments of the dust-forming regions and derive some basic properties of the freshly formed dust. The work was supported by the Projects of Distinction Fund of the Western Kentucky University. en Головна астрономічна обсерваторія НАН України Кинематика и физика небесных тел Plenary Sessions Winds of Wolf−Rayet stars: phenomenology of mass loss Article published earlier |
| spellingShingle | Winds of Wolf−Rayet stars: phenomenology of mass loss Marchenko, S.V. Plenary Sessions |
| title | Winds of Wolf−Rayet stars: phenomenology of mass loss |
| title_full | Winds of Wolf−Rayet stars: phenomenology of mass loss |
| title_fullStr | Winds of Wolf−Rayet stars: phenomenology of mass loss |
| title_full_unstemmed | Winds of Wolf−Rayet stars: phenomenology of mass loss |
| title_short | Winds of Wolf−Rayet stars: phenomenology of mass loss |
| title_sort | winds of wolf−rayet stars: phenomenology of mass loss |
| topic | Plenary Sessions |
| topic_facet | Plenary Sessions |
| url | https://nasplib.isofts.kiev.ua/handle/123456789/79404 |
| work_keys_str_mv | AT marchenkosv windsofwolfrayetstarsphenomenologyofmassloss |