scholarly journals Further Measurements of Stellar Temperatures and Planetary Radiation

1922 ◽  
Vol 8 (11) ◽  
pp. 330-333 ◽  
Author(s):  
W. W. Coblentz
Keyword(s):  
Stellar Temperatures

scholarly journals First inverse kinematics measurement of key resonances in the 22Ne(p,γ)23Na reaction at stellar temperatures

2020 ◽  
Vol 807 ◽  
pp. 135539 ◽  
Author(s):  
A. Lennarz ◽  
M. Williams ◽  
A.M. Laird ◽  
U. Battino ◽  
A.A. Chen ◽  
...  
Keyword(s):  
Inverse Kinematics ◽  
Stellar Temperatures

scholarly journals Tests of effective temperature – colour relations

1997 ◽  
Vol 189 ◽  
pp. 159-168
Author(s):  
R.A. Bell
Keyword(s):  
Globular Cluster ◽  
Effective Temperature ◽  
Average Difference ◽  
Flux Method ◽  
Synthetic Spectra ◽  
Stellar Temperatures ◽  
Angular Diameters

This paper discusses some tests of synthetic spectra used in the calculation of synthetic colours, as well as some of the problems which arise in these calculations. Synthetic colours are tested in two ways. Firstly, observed angular diameters of stars are compared with ones predicted from stellar temperatures derived from synthetic colours and the infrared flux method. The average difference is less than 2%. Secondly, a very metal-poor isochrone is transformed to the Mv, B–V and Mv, V–I colour planes and compared with observations of stars in the globular cluster M92. The agreement is good in both colour–magnitude diagrams.

Nucleosynthesis of Al-26 at low stellar temperatures

1983 ◽  
Vol 269 ◽  
pp. 686 ◽  
Author(s):  
A. E. Champagne ◽  
A. J. Howard ◽  
P. D. Parker
Keyword(s):  
Stellar Temperatures

scholarly journals A CO Search for Molecular Gas in High Mass Post-Main-Sequence Nebulae

1989 ◽  
Vol 120 ◽  
pp. 295-299
Author(s):  
J.P. Phillips ◽  
A. Mampaso ◽  
N. Ukita ◽  
P.G. Williams
Keyword(s):  
Main Sequence ◽  
Emission Measure ◽  
Rapid Evolution ◽  
Central Star ◽  
Physical Characteristics ◽  
High Mass ◽  
Molecular Gas ◽  
High Incidence ◽  
High Emission ◽  
Stellar Temperatures

High mass post-main-sequence nebulae are characterised by a set of unusual, and in certain cases extreme physical characteristics, including large outflow velocities (cf. Phillips and Mampaso, 1988a), extremely compact high emission measure cores (Phillips and Mampaso, 1988b), a high incidence of bipolar morphology (Peimbert and Torres Peimbert, 1982), and evidence for anomalously high levels of shock excited H2 S(l) emission towards both the source cores (Phillips et al 1983, 1985) and nebular peripheries (Zuckerman and Gatley, 1988). The large central star masses also predispose these sources to rapid evolution within the H-R plane (perhaps one or two orders of magnitude more rapid than for typical PN (Schonberner 1981, 1983), and the acquisition of stellar temperatures T* > 105 K, giving rise to correspondingly high levels of nebular excitation.

scholarly journals Absolute Calibration of Stellar Temperatures

1973 ◽  
Vol 54 ◽  
pp. 153-155
Author(s):  
H. Kienle ◽  
D. Labs
Keyword(s):  
Spectral Energy Distribution ◽  
Black Body ◽  
Absolute Temperature ◽  
Spectral Energy ◽  
Absolute Calibration ◽  
Standard Star ◽  
The Absolute ◽  
Stellar Temperatures ◽  
Image Position ◽  
Radiation Laboratory

The scale of effective temperatures Teff is based on observed absolute radiation temperatures Tr, which are defined by Planck's radiation law where TAu designs the absolute temperature of the gold point. A relative scale of radiation temperatures can be derived from spectrophotometric comparisons with a standard star. The absolute calibration of the standard star (α Lyr or Sun) demands a careful comparison with a standard radiation source of well known spectral energy distribution (Black Body or Synchrotron). With ground-based observations atmospheric extinction is to be taken into account; with extraterrestrial observations detectors may be used which are absolutely calibrated in a radiation laboratory under space conditions.

scholarly journals Effective Temperatures of Wolf-Rayet Stars

1973 ◽  
Vol 49 ◽  
pp. 54-56 ◽  
Author(s):  
Donald C. Morton
Keyword(s):  
Radio Emission ◽  
Central Star ◽  
Lyman Continuum ◽  
Astrophysical Journal ◽  
Direct Indication ◽  
H Ii Region ◽  
Effective Temperatures ◽  
Stellar Temperatures ◽  
Hydrogen Lines ◽  
Ring Nebulae

We have learned from Lindsey Smith's talk how useful it would be for our understanding of Wolf-Rayet stars to have reliable effective temperatures and bolometric corrections. The ring nebulae surrounding a few WN stars provide one method for estimating the stellar temperatures. I have assumed each nebula is a normal H ii region excited primarily by the Lyman continuum radiation of the central star. Then, if the nebula is optically thick shortward of 912 Å, each stellar photon with more energy than 13.6 eV is absorbed by the nebula and re-radiated in a predictable way as hydrogen lines and free-free radio emission. Consequently, nebular radio measures such as those recently obtained by Hugh Johnson (1971) provide a direct indication of the number of Lymancontinuum photons emitted by the central star. The exact equations have been described in the Astrophysical Journal (Morton, 1969; Morton, 1970).

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