scholarly journals THE WHITE DWARF POPULATION IN NGC 1039 (M34) AND THE WHITE DWARF INITIAL-FINAL MASS RELATION

2008 ◽  
Vol 135 (6) ◽  
pp. 2163-2176 ◽  
Author(s):  
Kate H. R. Rubin ◽  
Kurtis A. Williams ◽  
M. Bolte ◽  
Detlev Koester
Keyword(s):  
White Dwarf ◽  
Mass Relation ◽  
Final Mass

scholarly journals Constraining axion-like particles using the white dwarf initial-final mass relation

2021 ◽  
Vol 2021 (09) ◽  
pp. 010 ◽  
Author(s):  
Matthew J. Dolan ◽  
Frederick J. Hiskens ◽  
Raymond R. Volkas
Keyword(s):  
White Dwarf ◽  
Mass Relation ◽  
Final Mass

scholarly journals Central Stars of Planetary Nebulae in Galactic Open Clusters: Providing additional data for the White Dwarf Initial-to-Final-Mass Relation

2018 ◽  
Vol 14 (S343) ◽  
pp. 400-401
Author(s):  
Vasiliki Fragkou ◽  
Quentin A. Parker ◽  
Albert Zijlstra ◽  
Richard Shaw ◽  
Foteini Lykou
Keyword(s):  
White Dwarf ◽  
Additional Data ◽  
Open Cluster ◽  
Central Star ◽  
Open Clusters ◽  
Physical Parameters ◽  
Mass Relation ◽  
Carbon And Nitrogen ◽  
Final Mass ◽  
Central Stars

AbstractAccurate (< 10%) distances of Galactic star clusters allow a precise estimation of the physical parameters of any physically associated Planetary Nebula (PN) and also that of its central star (CSPN) and its progenitor. The progenitor’s mass can be related to the PN’s chemical characteristics and, furthermore, provides additional data for the widely used white dwarf (WD) initial-to-final mass relation (IFMR) that is crucial for tracing the development of both carbon and nitrogen in entire galaxies. To date, there is only one PN (PHR1315- 6555) confirmed to be physically associated with a Galactic open cluster (ESO 96 -SC04) that has a turn-off mass ∼2Mʘ. Our deep HST photometry was used for the search of the CSPN of this currently unique PN. In this work, we present our results.

Testing white dwarf cosmochronology using wide double white dwarfs

2019 ◽  
Vol 15 (S357) ◽  
pp. 197-201
Author(s):  
Tyler Heintz ◽  
JJ Hermes
Keyword(s):  
White Dwarf ◽  
White Dwarfs ◽  
Mass Relation ◽  
Final Mass ◽  
Gaia Dr2

AbstractWe present a sample of nearly 650 widely separated double white dwarf binaries found using Gaia DR2 astrometry. We derive preliminary total ages for each white dwarf in our sample using Gaia photometry and compare the total ages of both components of each binary in our sample. We find agreement within 3 sigma between the two ages ∼85% of the time with median age uncertainties of ∼3.5 Gyr depending on which initial-final mass relation is used. When a subsample with the most precise ages is used, the agreement within 3 sigma drops to ∼70% with median age uncertainties of 300-600 Myr.

scholarly journals The White Dwarf Initial–Final Mass Relation for Progenitor Stars from 0.85 to 7.5 M ⊙

2018 ◽  
Vol 866 (1) ◽  
pp. 21 ◽  
Author(s):  
Jeffrey D. Cummings ◽  
Jason S. Kalirai ◽  
P.-E. Tremblay ◽  
Enrico Ramirez-Ruiz ◽  
Jieun Choi
Keyword(s):  
White Dwarf ◽  
Mass Relation ◽  
Final Mass ◽  
Progenitor Stars

scholarly journals Carbon star formation as seen through the non-monotonic initial–final mass relation

2020 ◽  
Vol 4 (11) ◽  
pp. 1102-1110 ◽  
Author(s):  
Paola Marigo ◽  
Jeffrey D. Cummings ◽  
Jason Lee Curtis ◽  
Jason Kalirai ◽  
Yang Chen ◽  
...  
Keyword(s):  
Star Formation ◽  
Carbon Star ◽  
Mass Relation ◽  
Final Mass

scholarly journals Ensemble evolutionary studies of white dwarfs in open star clusters

2019 ◽  
Vol 15 (S357) ◽  
pp. 179-183
Author(s):  
Kurtis A Williams
Keyword(s):  
White Dwarfs ◽  
Binary Star ◽  
Open Cluster ◽  
Star Clusters ◽  
Mass Relation ◽  
Correlated Errors ◽  
Open Star Clusters ◽  
Open Star ◽  
Final Mass ◽  
Evolutionary Studies

AbstractWhite dwarfs (WDs) in open star clusters are a highly useful ensemble of stars. While numerous researchers use open cluster WDs to study the initial-final mass relation, numerous other evolutionary studies are also enabled by this sample of stars, including searches for stochastic mass loss, studies of binary star evolution, and measurements of metallicity impacts on WD formation and evolution. However, it is crucial to use astrometric data such as proper motions to remove contaminating field WDs from open cluster samples; multi-epoch ground based imaging is needed for most open cluster WDs. Also, the strongly correlated errors in the initial mass - final mass plane must be considered; we illustrate the importance of this consideration using a large open cluster WD sample and Monte Carlo techniques.

scholarly journals A Theory on the Slope of the IMF

1989 ◽  
Vol 120 ◽  
pp. 129-129
Author(s):  
H. Zinnecker
Keyword(s):  
Mass Spectrum ◽  
Molecular Clouds ◽  
Mass Relation ◽  
Final Mass ◽  
Co Observations ◽  
The Imf

Molecular clouds are clumpy, and the mass spectrum (dN/dM) of clumps scales with the clump mass M to the -1.5 power, as determined from CO observations of molecular clouds (Blitz 1988, Stutzki et al. 1989). The basic idea is to translate the mass spectrum of clumps into a mass spectrum of stars (that are assumed to form from these clumps) by virtue of a clump-star (i.e. initial-final) mass relation.

scholarly journals The Initial–Final Mass Relationship of White Dwarfs in Common Proper Motion Pairs and Open Clusters

2006 ◽  
Vol 2 (S240) ◽  
pp. 380-382
Author(s):  
S. Catalán ◽  
I. Ribas ◽  
J. Isern ◽  
E. García–Berro ◽  
C. Allende Prieto
Keyword(s):  
White Dwarf ◽  
Proper Motion ◽  
White Dwarfs ◽  
Open Clusters ◽  
Type Star ◽  
Spectroscopic Observations ◽  
Final Mass ◽  
Semi Empirical ◽  
Relationship Of

AbstractWe have studied white dwarfs in common proper motion pairs (CPMPs) to improve the semi-empirical initial–final mass relationship of white dwarfs. In this contribution, we report new results obtained from spectroscopic observations of both members of several CPMPs composed of an F, G or K type star and a DA white dwarf.

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