Zobrazeno 1 - 10
of 248 976
pro vyhledávání: '"Low Mass"'
Autor:
Ghosh, Rana1,2, Das, Ankan1,3, Gorai, Prasanta4,5 prasanta.astro@gmail.com, Mondal, Suman Kumar6, Furuya, Kenji7,8, Tanaka, Kei E. I.9, Takashi Shimonishi10, Fontani, Francesco11
Publikováno v:
Frontiers in Astronomy & Space Sciences. 2024, p01-25. 25p.
In the monograph, the authors systematize and generalize the results of studying solar-type activity that is characteristic of a significant part of mid- and low-mass stars of the Galaxy, outline the characteristics of such stars in the quiescent sta
Externí odkaz:
http://arxiv.org/abs/2411.11898
Autor:
Wadhwa, Surjit S., Landin, Natalia R., Arbutina, Bojan, Tothill, Nicholas F. H., De Horta, Ain Y., Filipovic, Miroslav D., Petrovic, Jelena, Djurasevic, Gojko
With the ever-increasing number of light curve solutions of contact binary systems increasing number of potential bright red nova progenitors are being reported. There remains, however, only one confirmed event. In the present study we undertake a co
Externí odkaz:
http://arxiv.org/abs/2411.02020
Autor:
Lim, Dongwook, Chun, Sang-Hyun, Lee, Young-Wook, Chung, Chul, Koch-Hansen, Andreas J., Hong, Seungsoo
Context. With the increasing number of discoveries of globular clusters in the inner Milky Way, the need for spectroscopic confirmation and further investigation of their stellar populations and chemodynamical properties has become crucial. Aims. Gra
Externí odkaz:
http://arxiv.org/abs/2410.21578
Autor:
Kuwahara, Ayumu, Lambrechts, Michiel, Kurokawa, Hiroyuki, Okuzumi, Satoshi, Tanigawa, Takayuki
The observed dust rings and gaps in protoplanetary disks could be imprints of forming planets. Even low-mass planets in the one-to-ten Earth-mass regime, that do not yet carve deep gas gaps, can generate such dust rings and gaps by driving a radially
Externí odkaz:
http://arxiv.org/abs/2410.16996
Autor:
Brito, Ana, Lopes, Ilídio
Publikováno v:
Astronomy & Astrophysics, 690, A228 (2024)
In the partially ionized material of stellar interiors, the strongest forces acting on electrons and ions are the Coulomb interactions between charges. The dynamics of the plasma as a whole depend on the magnitudes of the average electrostatic intera
Externí odkaz:
http://arxiv.org/abs/2410.10003
Autor:
van Gelder, M. L., Francis, L., van Dishoeck, E. F., Tychoniec, Ł., Ray, T. P., Beuther, H., Garatti, A. Caratti o, Chen, Y., Devaraj, R., Gieser, C., Justtanont, K., Kavanagh, P. J., Nazari, P., Reyes, S., Rocha, W. R. M., Slavicinska, K., Güdel, M., Henning, Th., Lagage, P. -O., Wright, G.
The MIRI-MRS instrument onboard JWST allows for probing the molecular gas composition at mid-IR wavelengths at unprecedented resolution and sensitivity. It is important to study these features in low-mass embedded protostellar systems since the forma
Externí odkaz:
http://arxiv.org/abs/2410.01636
Blue large-amplitude pulsators (BLAPs) are a recently discovered group of hot stars pulsating in radial modes. Their origin needs to be explained, and several scenarios for their formation have already been proposed. We investigate whether BLAPs can
Externí odkaz:
http://arxiv.org/abs/2410.00154
Autor:
McQuinn, Kristen B. W., Newman, Max J. B., Skillman, Evan D., Telford, O. Grace, Brooks, Alyson, Adams, Elizabeth A. K., Berg, Danielle A., Boyer, Martha L., Cannon, John M., Dolphin, Andrew E., Pahl, Anthony, Rhode, Katherine L., Salzer, John J., Cohen, Roger E., Goldman, Steve R.
Isolated, low-mass galaxies provide the opportunity to assess the impact of reionization on their star formation histories (SFHs) without the ambiguity of environmental processes associated with massive host galaxies. There are very few isolated, low
Externí odkaz:
http://arxiv.org/abs/2409.19050
Autor:
Partmann, Christian, Naab, Thorsten, Lahén, Natalia, Rantala, Antti, Hirschmann, Michaela, Hislop, Jessica M., Petersson, Jonathan, Johansson, Peter H.
Observed low-mass galaxies with nuclear star clusters (NSCs) can host accreting massive black holes (MBH). We present simulations of dwarf galaxies ($M_{\mathrm{baryon}} \sim 0.6 - 2.4 \times 10^8 \rm \, M_\odot$) at solar mass resolution ($0.5\rm \,
Externí odkaz:
http://arxiv.org/abs/2409.18096