Status: Bibliographieeintrag
Standort: ---
Exemplare:
---
| Online-Ressource |
Verfasst von: | Nayak, Omnarayani [VerfasserIn]  |
| Chevance, Mélanie [VerfasserIn]  |
Titel: | Stellar feedback on the earliest stage of massive star formation |
Verf.angabe: | O. Nayak, M. Meixner, Y. Okada, M.Y. Lee, M. Chevance, C. Buchbender, Y. Fukui, T. Onishi, A. Parikka, and J. Stutzki |
E-Jahr: | 2021 |
Jahr: | 2021 February 3 |
Umfang: | 12 S. |
Fussnoten: | Gesehen am 26.11.2021 |
Titel Quelle: | Enthalten in: The astrophysical journal / 1 |
Ort Quelle: | London : Institute of Physics Publ., 1996 |
Jahr Quelle: | 2021 |
Band/Heft Quelle: | 907(2021), 2, Artikel-ID 106, Seite 1-12 |
ISSN Quelle: | 1538-4357 |
Abstract: | We report SOFIA/GREAT observations of high-J CO lines and [C ii] observations of the super star cluster candidate H72.97-69.39 in the Large Magellanic Cloud (LMC), which is in its very early formation stage. We use our observations to determine if shocks are heating the gas or if photon-dominated regions (PDRs) are being heated by local far-UV radiation. We use a PDR model and a shock model to determine whether the CO and [C ii] lines arise from PDRs or shocks. We can reproduce the observed high-J CO and [C ii] emission with a clumpy PDR model with the following properties: a density of 104.7 cm−3, a mass of 104 M⊙, and UV radiation of 103.5 in units of Draine field. Comparison with the ALMA beam-filling factor suggests a higher density within the uncertainty of the fit. We find the lower-limit [C ii]/total infrared (TIR) ratio (ϵ) traced by [C ii]/TIR to be 0.026%, lower than other known young star-forming regions in the LMC. Our shock models may explain the CO (16−15) and CO (11−10) emission lines with shock velocity of 8-11 km s−1, pre-shock density of 104-105 cm−3, and GUV = 0 in units of Draine field. However, the [C ii] line emission cannot be explained by a shock model, thus it is originating in a different gas component. Observations of [O i] 63 μm predicted to be 1.1 × 10−13 W m−2 by PDR models and 7.8 × 10−15 W m−2 by shock models will help distinguish between the PDR and shock scenarios. |
DOI: | doi:10.3847/1538-4357/abcb89 |
URL: | Bitte beachten Sie: Dies ist ein Bibliographieeintrag. Ein Volltextzugriff für Mitglieder der Universität besteht hier nur, falls für die entsprechende Zeitschrift/den entsprechenden Sammelband ein Abonnement besteht oder es sich um einen OpenAccess-Titel handelt.
Volltext: https://doi.org/10.3847/1538-4357/abcb89 |
| DOI: https://doi.org/10.3847/1538-4357/abcb89 |
Datenträger: | Online-Ressource |
Sprache: | eng |
K10plus-PPN: | 1751208184 |
Verknüpfungen: | → Zeitschrift |
Stellar feedback on the earliest stage of massive star formation / Nayak, Omnarayani [VerfasserIn]; 2021 February 3 (Online-Ressource)
68712125