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Solid lines show ZZ Ceti instability strip (Van Grootel et al. 2013 ADS)
Dotted lines show empirical ZZ Ceti instability strip (Gianninas et al.
2011 ADS)
Dashed lines show V777 Her instability strip (Gilles Fontaine, private communication)
Plot properties
stars in the plot
( including unresolved double degenerates)
DA:
DB:
CND:
DC:
DQ:
DZ:
PG1159:
DO:
Other:
X axis:
minus
Flip X axis
Y axis:
minus
Flip Y axis
Dot radius:
Dot color:
X axis limits:
from:
to:
Y axis limits:
from:
to:
Histogram properties
objects used for histogram
( including unresolved double degenerates)
DA:
DB:
CND:
DC:
DQ:
DZ:
PG1159:
DO:
Other:
X axis:
X axis limit:
from:
to:
Y axis limit:
from:
to:
Bin width :
Options
objects used for histogram
( including unresolved double degenerates)
X axis limit:
from:
to:
Y axis limit:
from:
to:
Bin width (K):
Sun abundances were taken from Lodders, K. 2003,
Solar System Abundances and Condensation Temperatures of the Elements, ADS
Plot properties
stars in the plot
DA:
DB:
CND:
DC:
DQ:
DZ:
PG1159:
DO:
Other:
X axis:
log(
/
)
Y axis:
log(
/
)
Dot radius:
Dot color:
X axis limits:
from:
to:
Y axis limits:
from:
to:
Completeness
Assuming a local white dwarf density of
(pc-3), within pc we expect ~ stars.
Our database contains objects corresponding to %
completeness.
Logarithmic scale
The Montreal White Dwarf Database is produced and maintained by Prof. Patrick Dufour (Université de Montréal) and Dr. Simon Blouin (University of Victoria). Please send database updates, corrections, suggestions or bug reports to patrick.dufour@umontreal.ca.