Einstein Coefficients m Harry Kroto 2004

Einstein Coefficients m Harry Kroto 2004

Einstein Coefficients Bn←m m Harry Kroto 2004

Einstein Coefficients Bn←m m Harry Kroto 2004

Einstein Coefficients Bn←m Bn→m m Harry Kroto 2004

Einstein Coefficients Bn←m Bn→m m Harry Kroto 2004

Einstein Coefficients Bn←m Bn→m An→m m Harry Kroto 2004

Einstein Coefficients Bn←m Bn→m An→m m A = 1.2 x 10-37 3 n em2 transitions per sec Harry Kroto 2004

Einstein Coefficients Bn←m Bn→m An→m m A = 1.2 x 10-37 3 n em2 transitions per sec Spontaneous emission lifetime  Harry Kroto 2004

Einstein Coefficients Bn←m Bn→m An→m m A = 1.2 x 10-37 3 n em2 transitions per sec Spontaneous emission lifetime   (sec) = 1/A = 1037/3 sec Harry Kroto 2004

Lifetime (secs)  ~ 1037/3 Harry Kroto 2004

e = 1Debye 1yr = 3 x 107 sec * magnetic dipole   (Hz) 3 (Hz3)  (sec) H (1420 MHz) 21cm 1.5x109 3x1027 1010 * H2CO rotations 1cm 3 x 1010 3x1031 106 CO2 vibrations 10 3 x 1013 3 x 1040 10-3 Na D electronic 500nm 1.5 x 1014 6 x 1044 10-7 H Lyman  100nm 3 x 1015 3 x 1046 10-9 e = 1Debye 1yr = 3 x 107 sec * magnetic dipole Harry Kroto 2004

e = 1Debye 1yr = 3 x 107 sec * magnetic dipole   (Hz) 3 (Hz3)  (sec) H (1420 MHz) 21cm 1.5x109 3x1027 1010 * H2CO rotations 1cm 3 x 1010 3x1031 106 CO2 vibrations 10 3 x 1013 3 x 1040 10-3 Na D electronic 500nm 1.5 x 1014 6 x 1044 10-7 H Lyman  100nm 3 x 1015 3 x 1046 10-9 e = 1Debye 1yr = 3 x 107 sec * magnetic dipole Harry Kroto 2004

e = 1Debye 1yr = 3 x 107 sec * magnetic dipole   (Hz) 3 (Hz3)  (sec) H (1420 MHz) 21cm 1.5x109 3x1027 1010 * H2CO rotations 1cm 3 x 1010 3x1031 106 CO2 vibrations 10 3 x 1013 3 x 1040 10-3 Na D electronic 500nm 1.5 x 1014 6 x 1044 10-7 H Lyman  100nm 3 x 1015 3 x 1046 10-9 e = 1Debye 1yr = 3 x 107 sec * magnetic dipole Harry Kroto 2004

e = 1Debye 1yr = 3 x 107 sec * magnetic dipole   (Hz) 3 (Hz3)  (sec) H (1420 MHz) 21cm 1.5x109 3x1027 1010 * H2CO rotations 1cm 3 x 1010 3x1031 106 CO2 vibrations 10 3 x 1013 3 x 1040 10-3 Na D electronic 500nm 1.5 x 1014 6 x 1044 10-7 H Lyman  100nm 3 x 1015 3 x 1046 10-9 e = 1Debye 1yr = 3 x 107 sec * magnetic dipole Harry Kroto 2004

e = 1Debye 1yr = 3 x 107 sec * magnetic dipole   (Hz) 3 (Hz3)  (sec) H (1420 MHz) 21cm 1.5x109 3x1027 1010 * H2CO rotations 1cm 3 x 1010 3x1031 106 CO2 vibrations 10 3 x 1013 3 x 1040 10-3 Na D electronic 500nm 1.5 x 1014 6 x 1044 10-7 H Lyman  100nm 3 x 1015 3 x 1046 10-9 e = 1Debye 1yr = 3 x 107 sec * magnetic dipole Harry Kroto 2004

e = 1Debye 1yr = 3 x 107 sec * magnetic dipole   (Hz) 3 (Hz3)  (sec) H (1420 MHz) 21cm 1.5x109 3x1027 1010 * H2CO rotations 1cm 3 x 1010 3x1031 106 CO2 vibrations 10 3 x 1013 3 x 1040 10-3 Na D electronic 500nm 1.5 x 1014 6 x 1044 10-7 H Lyman  100nm 3 x 1015 3 x 1046 10-9 e = 1Debye 1yr = 3 x 107 sec * magnetic dipole Harry Kroto 2004

Collisions in the Interstellar Medium ISM In space the pressures are low Very low If n = number of molecules per cc (mainly H) then Harry Kroto 2004

Collisions in the Interstellar Medium ISM In space the pressures are low Very low If n = number of molecules per cc (mainly H) then 2b = 103/n yrs per collision Harry Kroto 2004

Collisions in the Interstellar Medium ISM In space the pressures are low Very low If n = number of molecules per cc (mainly H) then 2b = 103/n yrs per collision 3b = 1023/n2 yrs per collision Harry Kroto 2004

Collisions in the Interstellar Medium ISM In space the pressures are low Very low If n = number of molecules per cc (mainly H) then 2b = 103/n yrs per collision 3b = 1023/n2 yrs per collision Number densities are anything from n = 1-1000 Harry Kroto 2004

Harry Kroto 2004