B. Hansen

Publications177
h-index46
Citations7,875
Highly Influential Citations899
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Sloan digital sky survey: Early data release
The Sloan Digital Sky Survey (SDSS) is an imaging and spectroscopic survey that will eventually cover approximately one-quarter of the celestial sphere and collect spectra of ≈106 galaxies, 100,000…
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THE INITIAL-FINAL MASS RELATION : DIRECT CONSTRAINTS AT THE LOW-MASS END
The initial-final mass relation represents a mapping between the mass of a white dwarf remnant and the mass that the hydrogen-burning main-sequence star that created it once had. The empirical…
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Formation of the Terrestrial Planets from a Narrow Annulus
We show that the assembly of the Solar System terrestrial planets can be successfully modelled with all of the mass initially confined to a narrow annulus between 0.7 and 1.0 AU. With this…
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An age difference of two billion years between a metal-rich and a metal-poor globular cluster
TLDR
An absolute age of 9.9 ± 0.7 billion years is reported for the metal-rich globular cluster 47 Tucanae, determined by modelling the properties of the cluster’s white-dwarf cooling sequence, and provides quantitative evidence that metal- rich clusters like 47‬Tucanase formed later than metal-poor halo clusters like NGC‬6397.
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Stellar Evolution in NGC 6791: Mass Loss on the Red Giant Branch and the Formation of Low-Mass White Dwarfs* **
We present the first detailed study of the properties (temperatures, gravities, and masses) of the NGC 6791 white dwarf population. This unique stellar system is both one of the oldest (8 Gyr) and…
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The Masses of Population II White Dwarfs
Globular star clusters are among the first stellar populations to have formed in the Milky Way, and thus only a small sliver of their initial spectrum of stellar types are still burning hydrogen on…
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The White Dwarf Cooling Sequence of NGC6397
We present the results of a deep Hubble Space Telescope (HST) exposure of the nearby globular cluster NGC6397, focussing attention on the cluster's white dwarf cooling sequence. This sequence is…
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TESTING IN SITU ASSEMBLY WITH THE KEPLER PLANET CANDIDATE SAMPLE
We present a Monte Carlo model for the structure of low-mass (total mass <25 M ?) planetary systems that form by the in situ gravitational assembly of planetary embryos into final planets. Our model…
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A Young White Dwarf Companion to Pulsar B1620-26: Evidence for Early Planet Formation
TLDR
The color and magnitude of the stellar companion indicate that it is an undermassive white dwarf of age 480 × 106 ± 140 × 106 years, which places a constraint on the recent history of this triple system and supports a scenario in which the current configuration arose through a dynamical exchange interaction in the cluster core.
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The white dwarf cooling sequence of the globular cluster messier 4
We present the white dwarf sequence of the globular cluster M4, based on a 123 orbit Hubble Space Telescope exposure, with a limiting magnitude of V ~ 30 and I ~ 28. The white dwarf luminosity…
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