Spanish
Vol. 58 (2024), Contributions
Vol. 58 (2024)
Contributions

Feedback from Massive Star Winds

DOI: https://doi.org/10.22201/ia.14052059p.2024.58.09
J. M. Pittard
School of Physics and Astronomy, University of Leeds, Leeds, LS2 9JT, UK
M. M. Kupilas
School of Physics and Astronomy, University of Leeds, Leeds, LS2 9JT, UK. & School of Chemistry, University of Leeds, Leeds, LS2 9JT, UK.
C. J. Wareing
School of Physics and Astronomy, University of Leeds, Leeds, LS2 9JT, UK. & Department of Applied Mathematics, University of Leeds, Leeds, LS2 9JT, UK.
S. A. E. G. Falle
Department of Applied Mathematics, University of Leeds, Leeds, LS2 9JT, UK.
PDF
PDF

Keywords

galaxies: ISM
ISM: bubbles
ISM: kinematics and dynamics
stars: earlytype
stars: massive
stars: winds
outflows

How to Cite

Feedback from Massive Star Winds. (2024). Revista Mexicana De Astrofísica Y Astronomía Serie De Conferencias, 58, 27-29. https://doi.org/10.22201/ia.14052059p.2024.58.09
ACM ACS APA ABNT Chicago Harvard IEEE MLA Turabian Vancouver AMA

Download Citation

Endnote/Zotero/Mendeley (RIS) BibTeX

Abstract

Our current theoretical understanding of the impact of winds from massive stars on the interstellar medium (ISM) is reviewed. Such winds have the potential to be a significant source of momentum to the ISM. In practice, the momentum boost is highly sensitive to the degree of mixing between the hot shocked stellar wind material and surrounding or embedded colder gas. This mixing remains an ill-understood process. The range of possibilities that might exist is discussed.

Resumen

En esta contribución se revisa el conocimiento teórico actual del impacto que los vientos de estrellas masivas tienen en el medio interestelar (ISM). Dichos viento son potencialmente una importante fuente de momento al medio interestelar, pero en la práctica el aporte de momento depende fuertemente del grado de mezcla entre el material del viento chocado a altas temperaturas y el gas más frío que lo rodea o está embebido enél. Este proceso de mezcla permanece aún poco entendido. Aquí se discuten las diferentes posibilidades que pudieran existir.

Arthur S. J., Dyson J. E., Hartquist T. W., 1993, MNRAS, 261, 425
Arthur S. J., Henney W. J., Dyson J. E., 1996, A&A, 313, 897
Avedisova V. S., 1972, Soviet Ast. 15, 708
Castor J., McCray R., Weaver R., 1975, ApJ, 200, L107
Crowther P. A., et al., 2016, MNRAS, 458, 624
Dale J. E., Ngoumou J., Ercolano B., Bonnell I. A., 2014, MNRAS, 442, 694
Dyson J. E., de Vries J., 1972, A&A, 20, 223
El-Badry K., Ostriker E. C., Kim C.-G., Quataert E., Weisz D. R., 2019, MNRAS, 490, 1961
Falle S. A. E. G., 1975, A&A, 43, 323
Geen S., Rosdahl J., Blaizot J., Devriendt J., Slyz A., 2015, MNRAS, 448, 3248
Haid S., Walch S., Seifried D., Ẅunsch R., Dinnbier F., Naab T., 2018, MNRAS, 478, 4799
Harper-Clark E., Murray N., 2009, ApJ, 693, 1696
Hopkins, P., 2018, MNRAS, 477, 1578
Kruijssen J. M. D., et al. 2019, Nature, 569, 519
Lancaster L., Ostriker E. C., Kim J.-G., Kim C.-G., 2021a, ApJ, 914, 89
Lancaster L., Ostriker E. C., Kim J.-G., Kim C.-G., 2021b, ApJ, 914, 90
Lancaster L., Ostriker E. C., Kim J.-G., Kim C.-G., 2021c, ApJL, 922, L3
Pikelner S. B., 1968, Astrophys. Lett., 2, 97
Pittard J. M., Wareing C. J., Kupilas M. M., 2021, MNRAS, 508, 1768
Pittard J. M., 2022, MNRAS, 515, 1815
Rogers H., Pittard J. M., 2013, MNRAS, 431, 1337
Schneider F. R. N., et al., 2018, Science, 359, 69
Smartt S. J., 2015, PASA, 32, e016
Sukhbold T., Ertl T., Woosley S. E., Brown J. M., Janka H.-T., 2016, ApJ, 821, 38
Wareing C. J., Pittard J. M., Falle S. A. E. G., 2017, MNRAS, 465, 2757
Wareing C. J., Pittard J. M., Wright N. J., Falle S. A. E. G., 2018, MNRAS, 475, 3598
Weaver R., McCray R., Castor J., Shapiro P., Moore R., 1977, ApJ, 218, 377
Yan Z., Jerabkova T., Kroupa P., 2023, A&A, 670, A151

Similar Articles

start an advanced similarity search