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381
SN 2016ije: An SN 2002es-like Type Ia Supernova Exploded in a Metal-poor and Low-surface Brightness Galaxy
Published 2023-01-01“…These characteristics suggest that SN 2016ije might originate from the violent merger of a white dwarf binary system, when viewed near an orientation along the iron-group-element cavity caused by the companion star.…”
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382
OGLE-2014-BLG-0221Lb: A Jupiter Mass Ratio Companion Orbiting Either a Late-type Star or a Stellar Remnant
Published 2024-01-01“…Bayesian inference is used to estimate the physical parameters of the lens, revealing that the shorter timescale model predicts 65% and 25% probabilities of a late-type star and white dwarf host, respectively, while the longer timescale model favors a black hole host with a probability ranging from 60% to 95%, under the assumption that stars and stellar remnants have equal probabilities of hosting companions with planetary mass ratios. …”
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383
Probing the Low-mass End of Core-collapse Supernovae Using a Sample of Strongly-stripped Calcium-rich Type IIb Supernovae from the Zwicky Transient Facility
Published 2023-01-01“…They could evolve to form white dwarfs or explode as electron-capture supernovae (SNe) or iron core-collapse SNe (CCSNe). …”
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384
Asteroseismology and Spectropolarimetry of the Exoplanet Host Star λ Serpentis
Published 2023-01-01Get full text
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385
SN 2022joj: A Potential Double Detonation with a Thin Helium Shell
Published 2024-01-01“…Spectroscopically, we find strong agreement between SN 2022joj and double detonation models with white dwarf masses of around 1 M _⊙ and a thin He shell between 0.01 and 0.05 M _⊙ . …”
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386
JWST Low-resolution MIRI Spectral Observations of SN 2021aefx: High-density Burning in a Type Ia Supernova
Published 2023-01-01“…Emission line profiles and the presence of electron capture elements are used to constrain the mass of the exploding white dwarf (WD) and the chemical asymmetries in the ejecta. …”
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387
TOI-3984 A b and TOI-5293 A b: Two Temperate Gas Giants Transiting Mid-M Dwarfs in Wide Binary Systems
Published 2023-01-01“…TOI-3984 A ( J = 11.93) is an M4 dwarf hosting a short-period (4.353326 ± 0.000005 days) gas giant ( M _p = 0.14 ± 0.03 M _J and R _p = 0.71 ± 0.02 R _J ) with a wide-separation white dwarf companion. TOI-5293 A ( J = 12.47) is an M3 dwarf hosting a short-period (2.930289 ± 0.000004 days) gas giant ( M _p = 0.54 ± 0.07 M _J and R _p = 1.06 ± 0.04 R _J ) with a wide-separation M dwarf companion. …”
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388
PSR J2150+3427: A Possible Double Neutron Star System
Published 2023-01-01“…An estimate for the total mass of the system using the $\dot{\omega }$ gives M _tot = 2.59(13) M _⊙ , which is consistent with most of the known double neutron star (DNS) systems and one neutron star (NS)–white dwarf (WD) system named B2303+46. Combining $\dot{\omega }$ with the mass function of the system gives the masses of M _p < 1.67 and M _c > 0.98 M _⊙ for the pulsar and the companion star, respectively. …”
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389
The Initial Mass Function Based on the Full-sky 20 pc Census of ∼3600 Stars and Brown Dwarfs
Published 2024-01-01“…A complete accounting of nearby objects—from the highest-mass white dwarf progenitors down to low-mass brown dwarfs—is now possible, thanks to an almost complete set of trigonometric parallax determinations from Gaia, ground-based surveys, and Spitzer follow-up. …”
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390
Hunting for the progenitor of SN 1006: High resolution spectroscopic search with the FLAMES instrument
Published 2012“…It is widely believed that these events are the thermonuclear explosions of carbon-oxygen white dwarfs close to the Chandrasekhar mass (1.38 M\odot). …”
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391
Semi-analytical formulas for the Hertzsprung-Russell diagram
Published 2008-01-01“…This new technique is applied to the first 10 pc, the first 50 pc, the Hyades and to the determination of the distance of a cluster. The case of the white dwarfs is analyzed assuming the absence of calibrated data: our equation produces a smaller χ2 with respect to the standard color-magnitude calibration when applied to the Villanova Catalog of Spectroscopically Identified White Dwarfs. …”
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392
Preface of “Asymmetric Planetary Nebulae 8e”
Published 2022-07-01“…Planetary nebulae (PNe) are the progeny of low- and intermediate-mass stars, at the exact time in their late evolution when they eject their hydrogen-rich envelopes and start their transition towards white dwarfs [...]…”
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393
Stellar cooling limits on light scalar boson revisited
Published 2023-08-01“…We obtain limits on the Higgs-scalar mixing angle of 10−10–10−9, which are given by white dwarfs or red giants up to the luminosity limits, in the region where the scalar mass is lighter than about 10 keV.…”
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394
A two-stream formalism for the convective Urca process
Published 2005“…We conclude that the proper modelling of the Urca process is essential for determining the ignition conditions for the thermonuclear runaway in Chandrasekhar-mass white dwarfs.…”
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395
Analysis of the fractional relativistic polytropic gas sphere
Published 2023-08-01“…Abstract Many stellar configurations, including white dwarfs, neutron stars, black holes, supermassive stars, and star clusters, rely on relativistic effects. …”
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396
The formation of hydrogen-deficient stars in binaries
Published 2008“…Here I review the main binary interactions, stable and unstable mass transfer, binary mergers, and apply them to a variety of objects. including hot subdwarfs, He-rich sdO stars, AM CVn stars, Type Ia supernova progenitors, ultracool white dwarfs and Type Ic and gamma-ray burst progenitors.…”
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397
Galactic Model Parameters and Spatial Density of Cataclysmic Variables in the Gaia Era: New Constraints on Population Models
Published 2023-01-01“…A comparison of the luminosity function of white dwarfs with the luminosity function of all CVs in this study show that 500 times the luminosity function of CVs fits very well to the luminosity function of white dwarfs. …”
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398
The progenitors of sdB binaries: Confronting theory with observations
Published 2004“…We have re-examined the main binary evolution channels that produce sdB stars ( by stable and unstable mass transfer, the merging of two helium white dwarfs). We find that all three main channels are of comparable importance, but produce slightly different mass distributions and dominate at different times. …”
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399
Concluding remarks
Published 1999“…It is particularly important to study the evolutionary links between white dwarfs and subdwarf-B stars with stars considered to have been their progenitors, those on the Red Giant and Asymptotic Giant Branches. …”
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400
Supersoft X-ray sources as transient phases of cataclysmic variable evolution
Published 2001“…Such systems are concentrated in orbital period just above the period gap, and can, in the most favorable circumstances, achieve X-ray lifetimes in excess of 3 x 10(5) yr. They have white dwarfs of moderate mass (0.7 - 0.9 M.), and may therefore tend to lower X-ray temperatures and luminosities than the more populous, longer-period supersoft sources with donor masses exceeding similar to 1.5 M.. …”
Conference item