Zobrazeno 1 - 10
of 652 163
pro vyhledávání: '"Hot, P."'
Autor:
Bianchi, Luciana
Publikováno v:
ApJS, 2024, ID: ApJS - AAS54365
We present a catalog of 71,364 point-like UV sources with SDSS photometry and GALEX FUV-NUV less or equal 0.1mag. The limit corresponds to stellar Teff greater than 15,000 to 20,000K, slightly depending on gravity but nearly reddening-independent for
Externí odkaz:
http://arxiv.org/abs/2409.04626
Observational cosmology is rapidly closing in on a measurement of the sum M_nu of neutrino masses, at least in the simplest cosmologies, while opening the door to probes of non-standard hot dark matter (HDM) models. By extending the method of effecti
Externí odkaz:
http://arxiv.org/abs/2410.05815
The origin of Hot Jupiters (HJs) is disputed between a variety of in situ and ex situ formation scenarios. One of the early proposed ex situ scenarios was the Eccentric Kozai-Lidov (EKL) mechanism combined with tidal circularization, which can produc
Externí odkaz:
http://arxiv.org/abs/2408.13307
Aerosols are a ubiquitous feature of planetary atmospheres and leave clear spectral imprints in exoplanet spectra. Pre-JWST, exoplanet retrieval frameworks mostly adopted simple parametric approximations. With JWST, we now have access to mid-infrared
Externí odkaz:
http://arxiv.org/abs/2410.19253
Autor:
Pelletier, Stefan, Benneke, Björn, Chachan, Yayaati, Bazinet, Luc, Allart, Romain, Hoeijmakers, H. Jens, Lavail, Alexis, Prinoth, Bibiana, Coulombe, Louis-Philippe, Lothringer, Joshua D., Parmentier, Vivien, Smith, Peter, Borsato, Nicholas, Thorsbro, Brian
One of the outstanding goals of the planetary science community is to measure the present-day atmospheric composition of planets and link this back to formation. As giant planets are formed by accreting gas, ices, and rocks, constraining the relative
Externí odkaz:
http://arxiv.org/abs/2410.18183
Autor:
Sultan, Imran, Faucher-Giguère, Claude-André, Stern, Jonathan, Rotshtein, Shaked, Byrne, Lindsey, Wijers, Nastasha
The circumgalactic medium (CGM) in $\gtrsim 10^{12}$ $\mathrm{M}_{\odot}$ halos is dominated by a hot phase ($T \gtrsim 10^{6}$ K). While many models exist for the hot gas structure, there is as yet no consensus. We compare cooling flow models, in wh
Externí odkaz:
http://arxiv.org/abs/2410.16359
Presence of a hot corona above the accretion disc can have important consequences for the evolution of magnetic fields and the Shakura-Sunyaev (SS) viscosity parameter $\alpha$ in such a strongly coupled system. In this work, we have performed three-
Externí odkaz:
http://arxiv.org/abs/2410.14497
Hydrogen-rich white dwarfs (WDs) comprise the majority of the WD population, but are only rarely found at the very hot end of the WD cooling sequence. A small subgroup that exhibits both hydrogen and helium lines in their spectra, the so-called hybri
Externí odkaz:
http://arxiv.org/abs/2410.14345
In inertial confinement fusion (ICF) implosions, the preheating risks associated with hot electrons generated by laser plasma instabilities (LPI) are contingent upon the angular characteristics of these hot electrons for a given total energy. Using p
Externí odkaz:
http://arxiv.org/abs/2410.12460
Autor:
Sander, Andreas A. C.
The properties, impact, and fate of hot stars cannot be understood without considering their winds. Revealed to be an almost ubiquitous phenomenon in the regime of massive stars, the winds of hot stars arise from a complex physical mechanism that sti
Externí odkaz:
http://arxiv.org/abs/2410.12484