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pro vyhledávání: '"Kolecki, Jared R."'
Autor:
Wang, Ji, Kolecki, Jared R., Ruffio, Jean-Baptiste, Wang, Jason J., Mawet, Dimitri, Baker, Ashley, Bartos, Randall, Blake, Geoffrey A., Bond, Charlotte Z., Calvin, Benjamin, Cetre, Sylvain, Delorme, Jacques-Robert, Doppmann, Greg, Echeverri, Daniel, Finnerty, Luke, Fitzgerald, Michael P., Jovanovic, Nemanja, Liu, Michael C., Lopez, Ronald, Morris, Evan, Asnodkar, Anusha Pai, Pezzato, Jacklyn, Ragland, Sam, Roy, Arpita, Ruane, Garreth, Sappey, Ben, Schofield, Tobias, Skemer, Andrew, Venenciano, Taylor, Wallace, J. Kent, Wallack, Nicole L., Wizinowich, Peter, Xuan, Jerry W.
A benchmark brown dwarf (BD) is a BD whose properties (e.g., mass and chemical composition) are precisely and independently measured. Benchmark BDs are valuable in testing theoretical evolutionary tracks, spectral synthesis, and atmospheric retrieval
Externí odkaz:
http://arxiv.org/abs/2202.02477
Autor:
Kolecki, Jared R., Wang, Ji
With the launch of the JWST, we will obtain more precise data for exoplanets than ever before. However, this data can only inform and revolutionize our understanding of exoplanets when placed in the larger context of planet-star formation. Therefore,
Externí odkaz:
http://arxiv.org/abs/2112.02031
Autor:
Ishikawa, Hiroyuki Tako, Aoki, Wako, Hirano, Teruyuki, Kotani, Takayuki, Kuzuhara, Masayuki, Omiya, Masashi, Hori, Yasunori, Kokubo, Eiichiro, Kudo, Tomoyuki, Kurokawa, Takashi, Kusakabe, Nobuhiko, Narita, Norio, Nishikawa, Jun, Ogihara, Masahiro, Ueda, Akitoshi, Currie, Thayne, Henning, Thomas, Kasagi, Yui, Kolecki, Jared R., Kwon, Jungmi, Machida, Masahiro N., McElwain, Michael W., Nakagawa, Takao, Vievard, Sebastien, Wang, Ji, Tamura, Motohide, Sato, Bun'ei
Detailed chemical analyses of M dwarfs are scarce but necessary to constrain the formation environment and internal structure of planets being found around them. We present elemental abundances of 13 M dwarfs (2900 < Teff < 3500 K) observed in the Su
Externí odkaz:
http://arxiv.org/abs/2112.00173
Autor:
Kolecki, Jared R., Wang, Ji, Johnson, Jennifer A., Zinn, Joel C., Ilyin, Ilya, Strassmeier, Klaus G
By measuring the elemental abundances of a star, we can gain insight into the composition of its initial gas cloud -- the formation site of the star and its planets. Planet formation requires metals, the availability of which is determined by the ele
Externí odkaz:
http://arxiv.org/abs/2106.13251
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Akademický článek
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