Other
Scientific paper
Jun 1964
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1964bott....3..305j&link_type=abstract
Boletín de los Observatorios de Tonantzintla y Tacubaya Vol. 3, pp. 305-324 (1964) (http://www.astroscu.unam.mx/bott/)
Other
166
Stars: Atmospheres, Stars: Color-Magnitude Diagrams, Stars: General
Scientific paper
The infrared photometric program that was begun in 1959 has been continued and the time has come for a fairly extensive report on the progress of the work. This paper is divided into several sections, as follows: Observations. Photometric observations in ten wavelength bands, U, B, V, R, I, J, K, L, M and N, have been made. Some of these observations were made with the 82-inch and 36-inch telescopes of the McDonald Observatory and others were made by B. Iriarte with the 40-inch telescope of the Observatorio Astronómico Nacional of the University of Mexico but the majority were made with the 21-inch and 28-inch photometric telescopes of the Lunar and Planetary Laboratory (University of Arizona). Data for a total of 256 stars are given in this paper; of these, 241 have complete observations in U, B, V, R, I, J and K. Observations in L, M and N are given for a number of the brighter stars. For the R, I, J, K, L, M and N systems, the data here should be regarded as the standard values for additional photometric work. Intrinsic Colors of Stars. The data that are now available proved to be sufficient for the derivation of the intrinsic colors of many types of stars. These are giants of Luminosity Class III from G8 to M5, supergiants from O to M5 and main-sequence stars from O to K7. The intrinsic color-indices, U-V, B-V, V-R, V-I, V-J and V-K were derived for most types of stars within these ranges; in addition, V-L, V-M and V-N were derived for the ranges of spectral type and luminosity class for which data are available. Absolute Intensities and Bolometric Corrections. An absolute calibration procedure has made possible the derivation of the total energy outputs and these data were used to obtain the Bolometric Corrections for many types of stars for which intrinsic colors were derived. Effective Temperatures. The computed total energies have also been used, in conjunction with the apparent diameter measures that are available for ten stars, to derive the Effective Temperatures of many of the types of stars for which intrinsic colors are given. The Zero-Age Main Sequence (ZAMS) and Selected Stars. The Bolometric Corrections and Effective Temperatures were used to derive the M_{B} versus Log T_{e} diagram for the zero-age main sequence. This sequence has been extended to fainter stars by a number of M-dwarfs for which only R and R-I are yet available; however, the validity of this extension is open to question since there is some evidence that the few M-dwarfs that have so far been observed on this program may not be typical M-dwarfs, so far as their spectral-energy distributions are concerned. Three subdwarfs have been observed on this program; of these, two (τ Cet and Gmb 1830) have large trigonometric parallaxes. In the M_{B} versus Log T_{e} diagram, τ Cet falls exactly on the ZAMS while Gmb 1830 falls about 0.4 mag. below. Measures for the Future. The analysis of the present data has exposed three areas where more observational material is needed. These are: 1) We need more observations of M-dwarf stars in U, B, V, R, I, J and K. 2) More measures of stellar angular diameters are sorely needed. The intensity interferometer of Brown and Twiss will help for the early-type stars, but a new Michelson interferometer is needed for the cooler stars. 3) We need more and better observations at wavelengths shorter than 0.3 microns. Such measures can be made only from above the Earth's atmosphere.
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