Transport of gas from disk to halo in starforming galaxies
Using 3-D gas dynamic simulations, we study the supernova (SNe) driven transport of gas from the galactic disk. We assume that SNe are distributed randomly and uniformly in the galactic plane and we consider sufficiently high volume SNe rates that are typical for starforming galaxies: νSN = (0.3 − 3...
| Main Authors: | , , |
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| Format: | Article |
| Language: | English |
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De Gruyter
2017-12-01
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| Series: | Open Astronomy |
| Subjects: | |
| Online Access: | https://doi.org/10.1515/astro-2017-0025 |
| _version_ | 1818715367794540544 |
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| author | Shevchenko Mikhail G. Vasiliev Evgenii O. Shchekinov Yuri A. |
| author_facet | Shevchenko Mikhail G. Vasiliev Evgenii O. Shchekinov Yuri A. |
| author_sort | Shevchenko Mikhail G. |
| collection | DOAJ |
| description | Using 3-D gas dynamic simulations, we study the supernova (SNe) driven transport of gas from the galactic disk. We assume that SNe are distributed randomly and uniformly in the galactic plane and we consider sufficiently high volume SNe rates that are typical for starforming galaxies: νSN = (0.3 − 3) × 10−11 pc−3 yr−1. We found that under such conditions, a major part of gas locked initially in the galactic disk is transported up to ∼ 1 − 5 stellar scale heights within several millions years. As expected gas transport is more efficient in the case of a thinner stellar disk. An decrease/increase of SN rate in the galactic disk with the same stellar scale height leads to an enlarging/shortening of time scale for gas transport. Independent of SN rate, the major fraction of the swept up gas is in the cold phase (T < 103 K), though its volume filling factor is rather small, ∼1-3%. Hot gas with T > 106 K is elevated to larger heights than cold gas. |
| first_indexed | 2024-12-17T19:02:15Z |
| format | Article |
| id | doaj.art-428a9c3c502e4cb79fb9c809921acef2 |
| institution | Directory Open Access Journal |
| issn | 2543-6376 |
| language | English |
| last_indexed | 2024-12-17T19:02:15Z |
| publishDate | 2017-12-01 |
| publisher | De Gruyter |
| record_format | Article |
| series | Open Astronomy |
| spelling | doaj.art-428a9c3c502e4cb79fb9c809921acef22022-12-21T21:36:05ZengDe GruyterOpen Astronomy2543-63762017-12-0126122423210.1515/astro-2017-0025astro-2017-0025Transport of gas from disk to halo in starforming galaxiesShevchenko Mikhail G.0Vasiliev Evgenii O.1Shchekinov Yuri A.2Southern Federal University, Stachki Ave. 194, Rostov-on-Don 344090, Russian FederationSouthern Federal University, Stachki Ave. 194, Rostov-on-Don 344090, Russia; Special Astrophysical Observatory, RAS, Nizhnii Arkhyz, Karachaevo- Cherkesskaya Republic 369167, Russian FederationLebedev Physical Institute of Russian Academy of Sciences, ASC, Moscow 117997, Russia; Raman Research Institute, Sadashiva Nagar, Bangalore 560080, IndiaUsing 3-D gas dynamic simulations, we study the supernova (SNe) driven transport of gas from the galactic disk. We assume that SNe are distributed randomly and uniformly in the galactic plane and we consider sufficiently high volume SNe rates that are typical for starforming galaxies: νSN = (0.3 − 3) × 10−11 pc−3 yr−1. We found that under such conditions, a major part of gas locked initially in the galactic disk is transported up to ∼ 1 − 5 stellar scale heights within several millions years. As expected gas transport is more efficient in the case of a thinner stellar disk. An decrease/increase of SN rate in the galactic disk with the same stellar scale height leads to an enlarging/shortening of time scale for gas transport. Independent of SN rate, the major fraction of the swept up gas is in the cold phase (T < 103 K), though its volume filling factor is rather small, ∼1-3%. Hot gas with T > 106 K is elevated to larger heights than cold gas.https://doi.org/10.1515/astro-2017-0025galaxies: ism - ism: bubbles - shock waves - supernova remnants |
| spellingShingle | Shevchenko Mikhail G. Vasiliev Evgenii O. Shchekinov Yuri A. Transport of gas from disk to halo in starforming galaxies Open Astronomy galaxies: ism - ism: bubbles - shock waves - supernova remnants |
| title | Transport of gas from disk to halo in starforming galaxies |
| title_full | Transport of gas from disk to halo in starforming galaxies |
| title_fullStr | Transport of gas from disk to halo in starforming galaxies |
| title_full_unstemmed | Transport of gas from disk to halo in starforming galaxies |
| title_short | Transport of gas from disk to halo in starforming galaxies |
| title_sort | transport of gas from disk to halo in starforming galaxies |
| topic | galaxies: ism - ism: bubbles - shock waves - supernova remnants |
| url | https://doi.org/10.1515/astro-2017-0025 |
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