An independent method for determining the age of the universe

Winget, D. E.; Hansen, Christopher J.; Liebert, James; Horn, H. M. van; Fontaine, G.; Nather, R. E.; Kepler, S. O.; Lamb, D. Q.

doi:10.1086/184864

Cited by 414 publications

(289 citation statements)

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“…At low luminosities we can notice a sharp down-turn of the density of white dwarfs. This cut-off in the number counts has been interpreted by different authors (Winget et al 1987;García-Berro et al 1988) as the consequence of the finite age of the Galactic disk. Thus, a comparison between the theoretical luminosity functions and the observational data can provide information about the age of the Galactic disk.…”

Section: The Influence Of the Progenitorsmentioning

confidence: 92%

“…This is done by studying the influence of the initial-final mass relationship in the two fundamental tools typically used to statistically analyze the properties of the white dwarf population: the white dwarf luminosity function and the white dwarf mass distribution. It is important to realize that the former has also been consistently used to obtain estimates of the age of the Galactic disk (Dantona & Mazzitelli 1978;Winget et al 1987;García-Berro et al 1988;Richer et al 2000) and the past history of the galactic star formation rate (Noh & Scalo 1990;Díaz-Pinto et al 1994). The latter yields important information about the late stages of stellar evolution since it reveals the amount of mass lost during stellar evolution from an initial stellar mass distribution (Liebert et al 2005a).…”

Section: Motivation and Outline Of The Thesismentioning

confidence: 99%

“…This issue is important because a comparison of the theoretical white dwarf luminosity function and the observational data available can provide us with important information about both the star formation history (Noh & Scalo 1990;Díaz-Pinto et al 1994) and the age of the Galaxy (Winget et al 1987;García-Berro et al 1988), and because it depends on the initial-final mass relationship of white dwarfs, which is the main subject of this work.…”

Section: Introductionmentioning

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: The Influence Of the Progenitorsmentioning

confidence: 92%

Section: Motivation and Outline Of The Thesismentioning

confidence: 99%

Section: Introductionmentioning

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 potential of WDs as "cosmic clocks" had long been recognized (Schmidt (1959); Winget et al (1987);Wood (1992) Winget et al (1987)). Figure taken from (Liebert et al (1988)).…”

Section: Cool White Dwarfsmentioning

confidence: 99%

“…Beyond the maximum, the LF drops abruptly, this has been interpreted as due to the finite age of the galactic disk (Winget et al (1987)). The first cooling models by Winget et al (1987) derived an age of 9.3 Gyr for the galactic disk (later this value was modified by improved models). For a while this very optimistic view regarding the use of WDs as cosmic clocks prevailed (Fontaine et al (2001)).…”

Section: Cool White Dwarfsmentioning

confidence: 99%

Do Low Luminosity Stars Matter?

Ruíz

2009

Proc. IAU

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Abstract. Historically, low luminosity stars have attracted very little attention, in part because they are difficult to see except with large telescopes, however, by neglecting to study them we are leaving out the vast majority of stars in the Universe. Low mass stars evolve very slowly, it takes them trillions of years to burn their hydrogen, after which, they just turn into a He white dwarf, without ever going through the red giant phase. This lack of observable evolution partly explains the lack of interest in them. The search for the "missing mass" in the galactic plane turned things around and during the 60s and 70s the search for large M/L objects placed M-dwarfs and cool WDs among objects of astrophysical interest. New fields of astronomical research, like BDs and exoplanets appeared as spin-offs from efforts to find the "missing mass". The search for halo white dwarfs, believed to be responsible for the observed microlensing events, is pursued by several groups. The progress in these last few years has been tremendous, here I present highlights some of the great successes in the field and point to some of the still unsolved issues.

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Cool White Dwarfs

Kilic

2011

White Dwarf Atmospheres and Circumstellar Environments

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An independent method for determining the age of the universe

Cited by 414 publications

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Testing the Initial–Final Mass Relationship of White Dwarfs

Testing the Initial–Final Mass Relationship of White Dwarfs

Do Low Luminosity Stars Matter?

Cool White Dwarfs

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