lpetrich
Contributor
The Drake equation is astronomer Frank Drake's attempt to estimate how many communicative civilizations there are in our Galaxy.
Drake Equation | SETI Institute
NOVA | The Drake Equation
Carl Sagan on Drake Equation - YouTube
There have been lots of arguments about this equation and various modifications and extensions of it.
N = R* * fp * ne * fl * fi * fc * L
When Frank Drake proposed this equation in 1960, only R* was well-understood. But I think that we understand the other parameters a little bit better.
With the detection of numerous extrasolar planets, we are starting to get a handle of fp and ne. However, we have discovered some complications, like "hot Jupiters", giant planets much closer to their stars than what one would expect from the Solar System and their composition. Also, exoplanet detection has come very close to detecting Earthlike planets around Sunlike stars.
Exploration of the Solar System has also given some hints as to which planets could be habitable. Venus has a runaway greenhouse effect and Mars has evidence of a former ocean of liquid water. Europa, Ganymede, Callisto, Enceladus, Dione, and Titan likely have subsurface oceans, though those oceans may not have a kind of disequilibrium suitable for driving organisms' metabolism and growth.
With the variations in planetary systems that we have discovered, we may have to integrate over different star types -- red dwarfs seem to have different sorts of planetary systems than Sunlike stars.
There are still plenty of uncertainties, like how much water a habitable-zone Earthlike planet might have. Will it have much less than what the Earth has? It will then be a desert world with a very thin atmosphere. Will it have much more than what the Earth has? It will then have a superdeep ocean that covers all of its surface.
So fp is likely close to 1 while ne is still uncertain, though likely not much less than 1. Maybe 0.1 or 0.01 or 0.001.
Drake Equation | SETI Institute
NOVA | The Drake Equation
Carl Sagan on Drake Equation - YouTube
There have been lots of arguments about this equation and various modifications and extensions of it.
N = R* * fp * ne * fl * fi * fc * L
- N = number
- R* = rate of star formation in our Galaxy: stars/year
- fp = fraction of stars with planetary systems
- ne = number of planets in a planetary system suitable for life
- fl = fraction of habitable planets where life emerges
- fi = fraction of planets with life were intelligence emerges
- fc = fraction of planets with intelligence which have interstellar communicative ability
- L = lifetime as an interstellar communicator
When Frank Drake proposed this equation in 1960, only R* was well-understood. But I think that we understand the other parameters a little bit better.
With the detection of numerous extrasolar planets, we are starting to get a handle of fp and ne. However, we have discovered some complications, like "hot Jupiters", giant planets much closer to their stars than what one would expect from the Solar System and their composition. Also, exoplanet detection has come very close to detecting Earthlike planets around Sunlike stars.
Exploration of the Solar System has also given some hints as to which planets could be habitable. Venus has a runaway greenhouse effect and Mars has evidence of a former ocean of liquid water. Europa, Ganymede, Callisto, Enceladus, Dione, and Titan likely have subsurface oceans, though those oceans may not have a kind of disequilibrium suitable for driving organisms' metabolism and growth.
With the variations in planetary systems that we have discovered, we may have to integrate over different star types -- red dwarfs seem to have different sorts of planetary systems than Sunlike stars.
There are still plenty of uncertainties, like how much water a habitable-zone Earthlike planet might have. Will it have much less than what the Earth has? It will then be a desert world with a very thin atmosphere. Will it have much more than what the Earth has? It will then have a superdeep ocean that covers all of its surface.
So fp is likely close to 1 while ne is still uncertain, though likely not much less than 1. Maybe 0.1 or 0.01 or 0.001.