planck {astrolibR} | R Documentation |
Calculate the Planck function in units of ergs/cm2/s/A
planck (wave,temp)
wave |
wavelength(s) at which the Planck function is to be evaluated, in Angstroms, scalar or vectxor |
temp |
temperature of the Planck function, in degree K, scalar |
In this function, the wavelength data are converted to centimeters, and the Planck function is calculated for each wavelength point. See Allen (1973, sec 44) for more information.
If a star with a blackbody spectrum has a radius R and distance d, then the flux at Earth in erg/cm^2/s/A will be bbflux*R^2/d^2.
bbflux |
blackbody flux (i.e. pi*Intensity) at the specified wavelengths, in erg/cm^2/s/A |
Adapted from the IUE RDAF 1989
R adaptation by Arnab Chakraborty June 2013
Allen, C. W., "Astrophysical Quantities", Athlone Press, 3rd ed. http://adsabs.harvard.edu/abs/1973asqu.book.....A
# Calculate the blackbody flux at 30,000 K every 100 Angstroms between 2000A and 4000A wave = 2000 + seq(0,2000,by=100) plot(wave, planck(wave,30000), lty=1, lwd=2)