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17 results on '"John Hillier, D."'

1. X-Shooting ULLYSES: Massive stars at low metallicity. I. Project description

Author

Vink, Jorick S., primary, Mehner, A., additional, Crowther, P. A., additional, Fullerton, A., additional, Garcia, M., additional, Martins, F., additional, Morrell, N., additional, Oskinova, L. M., additional, St-Louis, N., additional, ud-Doula, A., additional, Sander, A. A. C., additional, Sana, H., additional, Bouret, J.-C., additional, Kubátová, B., additional, Marchant, P., additional, Martins, L. P., additional, Wofford, A., additional, van Loon, J. Th., additional, Grace Telford, O., additional, Götberg, Y., additional, Bowman, D. M., additional, Erba, C., additional, Kalari, V. M., additional, Abdul-Masih, M., additional, Alkousa, T., additional, Backs, F., additional, Barbosa, C. L., additional, Berlanas, S. R., additional, Bernini-Peron, M., additional, Bestenlehner, J. M., additional, Blomme, R., additional, Bodensteiner, J., additional, Brands, S. A., additional, Evans, C. J., additional, David-Uraz, A., additional, Driessen, F. A., additional, Dsilva, K., additional, Geen, S., additional, Gómez-González, V. M. A., additional, Grassitelli, L., additional, Hamann, W.-R., additional, Hawcroft, C., additional, Herrero, A., additional, Higgins, E. R., additional, John Hillier, D., additional, Ignace, R., additional, Istrate, A. G., additional, Kaper, L., additional, Kee, N. D., additional, Kehrig, C., additional, Keszthelyi, Z., additional, Klencki, J., additional, de Koter, A., additional, Kuiper, R., additional, Laplace, E., additional, Larkin, C. J. K., additional, Lefever, R. R., additional, Leitherer, C., additional, Lennon, D. J., additional, Mahy, L., additional, Maíz Apellániz, J., additional, Maravelias, G., additional, Marcolino, W., additional, McLeod, A. F., additional, de Mink, S. E., additional, Najarro, F., additional, Oey, M. S., additional, Parsons, T. N., additional, Pauli, D., additional, Pedersen, M. G., additional, Prinja, R. K., additional, Ramachandran, V., additional, Ramírez-Tannus, M. C., additional, Sabhahit, G. N., additional, Schootemeijer, A., additional, Reyero Serantes, S., additional, Shenar, T., additional, Stringfellow, G. S., additional, Sudnik, N., additional, Tramper, F., additional, and Wang, L., additional

Published
2023
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2. Database of CMFGEN Models in a 6-Dimensional Space

Author

Zsargó, Janos, Fierro, Celia Rosa, Klapp, Jaime, Arrieta, Anabel, Arias, Lorena, John Hillier, D., Diniz Junqueira Barbosa, Simone, Series editor, Chen, Phoebe, Series editor, Du, Xiaoyong, Series editor, Filipe, Joaquim, Series editor, Kara, Orhun, Series editor, Kotenko, Igor, Series editor, Liu, Ting, Series editor, Sivalingam, Krishna M., Series editor, Washio, Takashi, Series editor, Barrios Hernández, Carlos Jaime, editor, Gitler, Isidoro, editor, and Klapp, Jaime, editor

Published
2017
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10. The explosion of 9–29 M⊙ stars as Type II supernovae: Results from radiative-transfer modeling at one year after explosion.

Author

Dessart, Luc, John Hillier, D., Sukhbold, Tuguldur, Woosley, S. E., and Janka, H.-T.

Abstract

We present a set of nonlocal thermodynamic equilibrium steady-state calculations of radiative transfer for one-year-old Type II supernovae (SNe) starting from state-of-the-art explosion models computed with detailed nucleosynthesis. This grid covers single-star progenitors with initial masses between 9 and 29 M⊙, all evolved with the code KEPLER at solar metallicity and ignoring rotation. The [O I] λλ 6300, 6364 line flux generally grows with progenitor mass, and Hα exhibits an equally strong and opposite trend. The [Ca II] λλ 7291, 7323 strength increases at low 56Ni mass, at low explosion energy, or with clumping. This Ca II doublet, which forms primarily in the explosively produced Si/S zones, depends little on the progenitor mass but may strengthen if Ca+ dominates in the H-rich emitting zones or if Ca is abundant in the O-rich zones. Indeed, Si–O shell merging prior to core collapse may boost the Ca II doublet at the expense of the O I doublet, and may thus mimic the metal line strengths of a lower-mass progenitor. We find that the 56Ni bubble effect has a weak impact, probably because it is too weak to induce much of an ionization shift in the various emitting zones. Our simulations compare favorably to observed SNe II, including SN 2008bk (e.g., the 9 M⊙ model), SN 2012aw (12 M⊙ model), SN 1987A (15 M⊙ model), or SN 2015bs (25 M⊙ model with no Si–O shell merging). SNe II with narrow lines and a low 56Ni mass are well matched by the weak explosion of 9–11 M⊙ progenitors. The nebular-phase spectra of standard SNe II can be explained with progenitors in the mass range 12–15 M⊙, with one notable exception for SN 2015bs. In the intermediate mass range, these mass estimates may increase by a few M⊙, with allowance for clumping of the O-rich material or CO molecular cooling. [ABSTRACT FROM AUTHOR]

Published
2021
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12. Radiative-transfer models for explosions from rotating and non-rotating single WC stars

Author

Dessart, Luc, John Hillier, D., Yoon, Sung-Chul, Waldman, Roni, Livne, Eli, Laboratoire d'Astrophysique de Marseille (LAM), and Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)

Subjects
[PHYS]Physics [physics], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], ComputingMilieux_MISCELLANEOUS
Abstract

International audience

Published
2017

15. Inferring supernova IIb/Ib/Ic ejecta properties from light curves and spectra: correlations from radiative-transfer models.

Author

Dessart, Luc, John Hillier, D., Woosley, Stan, Livne, Eli, Waldman, Roni, Sung-Chul Yoon, and Langer, Norbert

Subjects
*SUPERNOVAE, *RADIATIVE transfer, *ASTRONOMICAL spectroscopy, *CURVILINEAR motion, *ELECTROMAGNETIC waves
Abstract

We present 1D non-local thermodynamic equilibrium time-dependent radiative-transfer simulations for a large grid of supernovae (SNe) IIb/Ib/Ic that result from the terminal explosion of the mass donor in a close-binary system. Our sample covers ejecta masses Me of 1.7-5.2 M☉, kinetic energies Ekin of 0.6-5.0×1051 erg, and 56Ni masses of 0.05-0.30M☉.We find a strong correlation between the 56Ni mass and the photometric properties at maximum, and between the rise time to bolometric maximum and the post-maximum decline rate.We confirm the small scatter in (V - R) at 10 d past R-band maximum. The quantity Vm ≡ √ 2Ekin/Me is comparable to the Doppler velocity measured from He I 5875 Å at maximum in SNe IIb/Ib, although some scatter arises from the uncertain level of chemical mixing. The OI 7772 Å line may be used for SNe Ic, but the correspondence deteriorates with higher ejecta mass/energy. We identify a temporal reversal of the Doppler velocity at maximum absorption in the ~1.05 μm feature in all models. The reversal is due to He I alone and could serve as a test for the presence of helium in SNe Ic. Because of variations in composition and ionization, the ejecta opacity shows substantial variations with both velocity and time. This is in part the origin of the offset between our model light curves and the predictions from the Arnett model. [ABSTRACT FROM AUTHOR]

Published
2016
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