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Feedback from the Vicinity of Massive Protostars in the First Star Formation

Published online by Cambridge University Press:  20 January 2023

Kazutaka Kimura Open the ORCID record for Kazutaka Kimura [Opens in a new window]
Kazutaka Kimura*
Affiliation:
Center for Gravitational Physics and Quantum Information, Yukawa Institute for Theoretical Physics, Kyoto University, Kyoto 606-8502, Japan
*
email: [email protected]
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Abstract

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Many simulations have been performed to elucidate the formation process of first stars. In first star formation, radiative feedback is a key process in determining stellar masses. However, previous simulations which follow the feedback process don’t resolve the small scale ( 10 AU) to realize long-term calculation, and the structure near massive protostars is still unknown. To clarify how the radiation from the protostar works, we need to resolve small scale and calculate the interaction between the radiation and the dense gas in such a region. As a first step towards understanding the phenomenon in this region, we perform the high-resolution simulation around the massive protostar without radiative transfer. We find that dense gas covers the protostar even in the polar direction and the HII region cannot expand. Solving the radiative transfer for getting accurate results is our future work. We are currently developing the new radiation hydrodynamics code for that.

Keywords

stars: formationaccretionaccretion disksHII regions
Type
Contributed Paper
Information
Proceedings of the International Astronomical Union , Volume 16 , Symposium S362: The Predictive Power of Computational Astrophysics as a Discovery Tool , June 2020 , pp. 246 - 249
Copyright
© The Author(s), 2023. Published by Cambridge University Press on behalf of International Astronomical Union

References

Federrath, C., Banerjee, R., Clark, P. C., Klessen, R. S., 2010, ApJ, 713, 269 10.1088/0004-637X/713/1/269CrossRefGoogle Scholar
Greif, T. H. 2015, Computational Astrophysics and Cosmology, 2, 3 10.1186/s40668-014-0006-2CrossRefGoogle Scholar
Haemmerlé, Mayer, Klessen, Hosokawa, Madau, & Bromm, 2020, SSRv, 216, 4810.1007/s11214-020-00673-yCrossRefGoogle Scholar
Hirano, S., Hosokawa, T., Yoshida, N., et al. 2014, ApJ, 781, 60,10.1088/0004-637X/781/2/60CrossRefGoogle Scholar
Hirano, S., Hosokawa, T., Yoshida, N., Omukai, K., & Yorke, H. W. 2015, MNRAS, 448, 568 10.1093/mnras/stv044CrossRefGoogle Scholar
Hosokawa, T., Omukai, K., Yoshida, N., & Yorke, H. W. 2011, Science, 334, 1250 10.1126/science.1207433CrossRefGoogle Scholar
Kimura, K., Hosokawa, T., Sugimura, K. 2021, ApJ, 911, 52 10.3847/1538-4357/abe866CrossRefGoogle Scholar
Matsukoba, R., Takahashi, S. Z., Sugimura, K., & Omukai, K. 2019, MNRAS, 484, 2605 10.1093/mnras/sty3522CrossRefGoogle Scholar
McKee, C. F., & Tan, J. C. 2008, ApJ, 681, 771 10.1086/587434CrossRefGoogle Scholar
Sharda, P., Federrath, C., Krumholz, M. R., Schleicher, D. R. G., 2021, MNRAS (Letters), 503, 2014 Google Scholar
Sugimura, K., Matsumoto, T., Hosokawa, T., Hirano, S., & Omukai, K. 2020, ApJ (Letters), 892, L14 Google Scholar
Takahashi, S. Z., & Omukai, K. 2017, MNRAS, 472, 532 10.1093/mnras/stx1988CrossRefGoogle Scholar