by hippietrekx » Sat Jun 26, 2010 2:30 am
White dwarfs, earth-sized stars of degenerate matter, are suspected to come into
existence as asymptotic giant stars release their envelopes in a massive stellar
wind. If the star has mass beneath a certain threshold (approximately eight solar
masses), the star blows o these outer layers before the degenerate core begins
the runaway fusion process that leads to supernovae. White dwarfs can form
prematurely, resulting in what are known as low-mass white dwarfs. Theory
suggests that such objects form when a red giant is stripped of its envelope
before helium fusion begins (Hansen 2005). This project serves to seek further
evidence regarding how these red giants lose their outer envelopes.
Stellar evolutionary theory attributes such rapid losses of mass to the evo-
lution of interacting binary systems, where the more massive star over
ows its
Roche Lobe when it reaches the red giant phase. If the two stars are within
a few solar radii, this leads to a common envelope phase, where the envelope
of the red giant consumes the companion. As the companion star continues to
fuse hydrogen, the companion's luminosity expels the outer layers of the star,
leaving a white dwarf star and a main sequence star (Kilic 2010).
Observations of the open star cluster NGC 6791 suggest that this metal-rich
cluster houses numerous white dwarfs with masses below the expected limit
(0.45 solar masses) for single white dwarfs (Hansen 2005). Although these stars
could be the result of interacting binaries, the plethora of these dwarfs of mass
less than 0.45 solar masses within the cluster challenges such an allegation.
The binary mass fraction of NGC 6791, insucient to account for the number
of these objects, suggests a supplementary theory that these low-mass white
dwarfs can form in alternate environmental conditions, particularly in metal-
rich environments (Kilic et al. 2007).
A recent survey of more local white dwarfs marked by strong hydrogen ab-
sorption lines remarks that nearly all low-mass white dwarfs are expected to
exist in a binary system (Liebert et al. 2005). Despite such calculations, a siz-
able fraction (near 30 %) of suspected companions of the white dwarfs examined
have yet to be detected (Kilic 2007). Liebert argues that such results may arise
1
from the lack of available techniques in the detection of certain companions, yet
the consistent absence of detectable companions suggests otherwise.
We will provide radial velocity analysis of 21 low-mass white dwarfs, search-
ing for single white dwarfs that may have arisen as the end-result of metal-rich
stellar evolution. Beginning with descriptions of observations and of data anal-
ysis techniques, this paper will focus on each object, providing detailed records
of the likelihood of a companion and other characteristic qualities of the stars
that may assist in theorizing their formation.