Spectropolarimetric Survey of Hydrogen‐rich White Dwarf Stars

Kawka, A.; Vennes, S.; Schmidt, Gary D.; Wickramasinghe, D. T.; Koch, R.

doi:10.1086/509072

Cited by 190 publications

(292 citation statements)

References 99 publications

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“…The results of that study are compatible with the masses derived in this work except for WD1544−377, whose mass is 25% smaller when calculated from its gravitational redshift. However, Kawka et al (2007) inferred the spectroscopic mass of this star, together with those of WD1620−391 and WD1659−531, that are in good agreement with our results. WD0913+442 was studied by Karl et al (2005) and Bergeron et al (2001).…”

Section: Masses and Cooling Timessupporting

confidence: 90%

“…On the other hand, the southern hemisphere targets had been also studied by different authors. Recently, Kawka et al (2007) derived the atmospheric parameters of WD1544−377, WD1620−391 and WD1659−531, which are in good agreement with our results. …”

Section: Atmospheric Parameterssupporting

confidence: 89%

“…Some of the white dwarfs in our sample have been the subject of these kind of studies to confirm or discard their magnetic nature. Kawka et al (2007) obtained circularly polarized spectra of WD0413−017, WD1544−377, WD1620−391 and WD1659−531, finding evidence of magnetism only for the first of these stars. This result is in good agreement with the findings of other authors (Fabrika et al 2000;Aznar Cuadrado et al 2004;Jordan et al 2007).…”

Section: Discussionmentioning

confidence: 99%

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Testing the Initial–Final Mass Relationship of White Dwarfs

Catalán

Isern

Garcı́a–Berro

et al. 2010

Astrophysics and Space Science Proceedings

113

184

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A mis padres y hermana AgraïmentsEn primer lloc vull agrair als meus directors de tesi, Jordi Isern i Enrique García-Berro, que em donessin l'oportunitat de realitzar el doctorat a l'IEEC (al CSIC i a la UPC), així com que em proporcionessin tot el suport necessari. Crec que he après moltes coses importants en aquestsúltims anys, no només en la part científica, i això en partés una conseqüència d'haver treballat amb ells. Els vull donar les gràcies també pel suport i la confiança dipositada en mi, especialment durant aquestúltim any de feina.Durant tota aquestaèpoca he tingut la sort de tenir uns companys fantàstics que m'han fet molt més fàcil la feina. Primer vaig conèixer l'Alina, la meva companya de "fatigas" i després el Jose, el Pep i el Miquel. Més tard s'hi van afegir l'Ignasi, la Violeta, l'Anna C., l'Anna A., el Carlo, el Moi, el Nil, l'Anaïs. . . Tots els moments que hem compartit dins i fora de l'IEEC han estat molt importants per a mi i m'emporto un gran record de tota aquestaèpoca, primer al Nexus, després a la UAB i finalment a l'ETSE. Ara que tinc la oportunitat, els hi vull agrair als meus companys, o més ben dit, amics, tots elsànims i suport que m'han donat. També els hi vull donar les gràcies al personal d'administració i a la resta de companys que he tingut durant aquests anys.En especial, l'Ignasi es mereix un gran gràcies. . . Primer de tot, per venir a l'IEEC en un moment en que la meva feina necessitava d'un observador amb experiència. Per tenir la generositat de compartir els seus coneixements amb mi durant aquests anys, per acompanyar-me en les observacions, per tenir sempre tanta confiança en mi, molta més que jo mateixa i per ajudar-me sempre que se li presentés la oportunitat. Els seusànims i el seu suport han estat essencials per a que arribés aquest moment i per tant, només em queda donar-li el meu agraïment més sincer.También le debo un agradecimiento especial a Carlos Allende Prieto, que sin ni siquiera conocerme en persona aceptó acompañarme a observar al McDonald Observatory durante 10 días. Su ayuda y dedicación en la distancia, especialmente en el análisis de las compañeras de las enanas blancas, han sido también vitales para el desarrollo de esta tesis.Durante mi doctorado he tenido la oportunidad de disfrutar de estancias en otros centros. Le quiero dar las gracias a Inma Domínguez, Carlos Abia y Olga Zamora de la Universidad de Granada por la atención que me dispensaron cuando estuve allí. También quisiera dar las gracias a Roberto Silvotti y Juan Alcalá por la ayuda y el buen trato que me dieron durante el tiempo que pasé en el Osservatorio Astronomico di Capodimonte. Gracias también al resto de personas que trabajan en el Osservatorio y que hicieron mi estancia muy agradable.A mi profesor Manolo Segura le quiero agredecer que en su día me hiciera creer en mis posibilidades y despertara mi afán por intentar superarme poco a poco. Muchas gracias también por la "contingencia" y por la confianza dipositada en mí.En un momento para mí tan importante comoéste no me puedo olvi...

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Section: Masses and Cooling Timessupporting

confidence: 90%

Section: Atmospheric Parameterssupporting

confidence: 89%

Section: Discussionmentioning

confidence: 99%

See 1 more Smart Citation

Testing the Initial–Final Mass Relationship of White Dwarfs

Catalán

Isern

Garcı́a–Berro

et al. 2010

Astrophysics and Space Science Proceedings

113

184

View full text Add to dashboard Cite

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“…The different curves correspond to the effective temperatures 30 000-50 000 K. Since we cannot strictly estimate the extrapolation error we visually added some uncertainty to the extrapolated values, which was subsequently used to estimate the errors in Table 6. 1 Using the visual magnitude from Barstow et al (1995); 2 using the visual magnitude from Kawka et al (2007).…”

Section: Mass and Radius Determinations Of Re J 0317-853 And Lb 9802mentioning

confidence: 99%

“…The Guide Star Catalogue-II is a joint project of the Space Telescope Science Institute and the Osservatorio Astronomico di Torino. the highest known temperature of all MWDs with a field strength above 20 MG (Kawka et al 2007;Külebi et al 2009). Barstow et al (1995) performed high-speed photometry demonstrating that the optical brightness of RE J 0317-853 varies almost sinusoidally with a period of 725.4 ± 0.9 s and an amplitude of more than 0. m 1; these results were confirmed by Vennes et al (2003), who inferred a period of 725.727 ± 0.001 s from the variation in the circular polarisation.…”

Section: Introductionmentioning

confidence: 99%

Constraints on the origin of the massive, hot, and rapidly rotating magnetic white dwarf RE J 0317-853 from an HST parallax measurement

Külebi

Jordan

Nelan

et al. 2010

A&A

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Aims. We use the parallax measurements of RE J 0317-853 to determine its mass, radius, and cooling age and thereby constrain its evolutionary origins. Methods. We observed RE J 0317-853 with the Hubble Space Telescope's Fine Guidance Sensor to measure the parallax of RE J 0317-853 and its binary companion, the non-magnetic white dwarf LB 9802. In addition, we acquired spectra of comparison stars with the Boller & Chivens spectrograph of the SMARTS telescope to correct the parallax zero point. For the corrected parallax, we determine the radius, mass, and the cooling age with the help of evolutionary models from the literature. Results. The properties of RE J 0317-853 are constrained using the parallax information. We discuss the different cases of the core composition and the uncertain effective temperature. We confirm that RE J 0317-853 is close to the Chandrasekhar's mass limit in all cases and almost as old as its companion LB 9802.Conclusions. The precise evolutionary history of RE J 0317-853 depends on our knowledge of its effective temperature. It is possible that it had a single star progenitor possible if we assume that the effective temperature is at the cooler end of the possible range from 30 000 to 50 000 K; if T eff is instead at the hotter end, a binary-merger scenario for RE J 0317-853 becomes more plausible.

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White Dwarf Stars in the Big Data Era

Camisassa

2024

Astron Nachr

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White dwarf stars are the most common endpoint of stellar evolution. Therefore, these old, numerous and compact objects provide valuable information on the late stages of stellar evolution, the physics of dense plasma and the structure and evolution of our Galaxy. The ESA Gaia space mission has revolutionized this research field, providing parallaxes and multi‐band photometry for nearly 360,000 white dwarfs. Furthermore, this data, combined with spectroscopical and spectropolarimetric observations, have provided new information on their chemical abundances and magnetic fields. This large data set has raised new questions on the nature of white dwarfs, boosting our theoretical efforts for understanding the physics that governs their evolution and for improving the statistical analysis of their collective properties. In this article, I summarize the current state of our understanding of the collective properties of white dwarfs, based of detailed theoretical models and population synthesis studies.

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Spectropolarimetric Survey of Hydrogen‐rich White Dwarf Stars

Cited by 190 publications

References 99 publications

Testing the Initial–Final Mass Relationship of White Dwarfs

Testing the Initial–Final Mass Relationship of White Dwarfs

Constraints on the origin of the massive, hot, and rapidly rotating magnetic white dwarf RE J 0317-853 from an HST parallax measurement

White Dwarf Stars in the Big Data Era

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