Calculating the Habitable Zone
A General Method for Approximating the Habitable Zone around a Main Sequence Star
Tom Morris
Professor Emeritus of Biology
Natural Sciences Division
Fullerton College
Fullerton, CA
USA
PlanetaryBiology.com
October 2010 (refreshed July 2023)
Get this procedure in *.pdf format.
Two stages of calculations
Stage 1: Estimate the host star’s absolute luminosity based on the star’s apparent visual magnitude
First Step (stage 1) – Calculate the absolute visual magnitude of the host star based on the star’s apparent magnitude.
Mv = mv – 5 log(d/10)
Where:
Mv = Absolute magnitude of the star
mv = apparent magnitude of the star (visual spectrum)
d = distance from Earth to the star in parsecs
Second Step (stage 1) – Calculate bolometric magnitude of the host star.
Mbol = Mv + BC
Where:
Mbol = bolometric magnitude of the star
Mv = the absolute magnitude of the star
BC = bolometric correction constant
Use the following table for general bolometric correction values [generalized from Habets and Heintz (1981)]
Spectral class |
BC |
B |
-2.0 |
A |
-0.3 |
F |
-0.15 |
G |
-0.4 |
K |
-0.8 |
M |
-2.0 |
Third Step (stage 1) – Calculate the absolute luminosity of the host star
Lstar/Lsun = 
Where:
Lstar/Lsun = the absolute luminosity of the host star in terms of the absolute luminosity of the sun
Mbol star = the bolometric magnitude of the host star
Mbol sun = the bolometric magnitude of the sun = 4.72
2.5 is a constant value used for comparing stellar luminosities -- known as "Pogson's Ratio."
Stage 2: Approximate the radii of the boundaries of the host star’s habitable zone
Where:
This method approximates habitable zone radii using stellar luminosity and stellar flux following methods presented by Whitmire et al., 1996, cited below.
ri = the inner boundary of the habitable zone in astronomical units (AU)
ro = the outer boundary of the habitable zone in astronomical units (AU)
Lstar is the absolute luminosity of the star
1.1 is a constant value representing stellar flux at the inner radius (based on Kasting et al., 1993, cited below; Whitmire et al., 1996, cited below)
0.53 is a constant value representing stellar flux at the outer radius (based on Kasting et al., 1993, cited below; Whitmire et al., 1996., cited below)
Example
- Star = Kepler-22
- mv = 12
- Spectral type = G5 V
- BC = -0.4 (based on G class star, and approximated using value in above table)
- Distance = 190 parsecs
1. Calculate absolute visual magnitude
Mv = 12 – 5log(190/10) = 5.6
2. Calculate bolometric magnitude
Mbol = 5.6 + (-0.4) = 5.2
3. Calculate absolute luminosity
4. Approximate the boundaries of the habitable zone for this star
For more information on the development of this methodology, please consult the refences listed below, and see the chapter entitled "Astronomical Circumstances" in Principles of Planetary Biology
References
- Fogg, Martyn J., (1992). An estimate of the prevalence of biocompatible and habitable planets. Journal of the British Interplanetary Society, 45: 3-12.
- Habets, G.M.H.J.; Heintze, J.R.W., (1981). Empirical bolometric corrections for the main sequence. Astron. Astrophys. Suppl. Ser. 46: 193-237.
- Kasting, James; Whitmire, Daniel; and Reynolds, Ray (1993). Habitable zones around main sequence stars. Icarus 101: 108-128.
- Kasting, James F. (1996). Habitable zones around stars: An update. In: Doyle, Laurence (ed.). Circumstellar Habitable Zones, 117-142. Travis House Publications, Menlo Park.
- Lang, Kenneth (1992). Astrophysical Data: Planets and Stars. Springer-Verlag, New York.
- Whitmire, Daniel; Reynolds, Ray, (1996). Circumstellar habitable zones: astronomical considerations. In: Doyle, Laurence (ed.). Circumstellar Habitable Zones, 117-142. Travis House Publications, Menlo Park. Available for download from this site (with my notes)
An alternative approach has been proposed by:
"Habitable Zones Around Main-Sequence Stars: New Estimates" by Kopparapu et al.(2013), Astrophysical Journal, 765, 131
Try the online habitable zone caclulator based on this alternative approach at: