Scott J. Wolk
can be derived from simple arguments
about stars on the Hayashi track. The potential energy given
off by stars on this track is 17#17, while the stellar
luminosity 18#18. Since the stellar luminosity is
the change in energy per unit time,
19#19. Along the
convective tracks, temperature is approximately constant. Removing all
the constants one gets 20#20.
Integrating leads to 21#21.
- The Image Reduction and Analysis Facility is distributed
by the National Optical Astronomy Observatories.
- The usage of S/N in this context is not the same as in
standard photometry. ``Noise'' has the same meaning, but here ``signal''
refers to the intrinsic strength of the modulation. If a star is measured to
2 accuracy and has at 10 modulation (0.2 magnitudes peak to peak),
the S/N is 5.
- The sensitivity limit varied from field to field on
the basis on the brightest available field standard star. The mean noise
level in the field standards was about 5.
- Edwards et al.
uses H-K=0.2 as their cut off for stars without disks. I use 0.4 as
an upper limit because the errors in H-K can be 213#213 0.1.
- It is still possible to plug the cord
to the drive in upside-down. The operator should take care in
placing this plug.
accuracy of the results presented Tables and
is often limited by the resolution of the grid used for our
simulations. In many cases, the last digit tabulated should not be
regarded as significant, so results which appear to be identical to
four places despite differing input parameters may only have been
the same to three places if a higher resolution code were used. However,
given the scatter in the observational data, we do not believe that
more precise modeling is warranted.
Mon Nov 25 15:41:03 EST 1996