In contrast the spectrum shows a higher excitation temperature closer to the equatorial plane.
2.
The excitation temperature varies across the Helix nebula.
3.
The excitation temperature can even be negative for a system with inverted levels ( such as a maser ).
4.
Thus the excitation temperature is the temperature at which we would expect to find a system with this ratio of level populations.
5.
In observations of the 21 cm line, the apparent value of the excitation temperature is often called the " spin temperature ".
6.
He continued his studies at the University of Canterbury and earned his M . Sc . in Physics in August 1979 . His master s thesis was titled Excitation Temperatures for Late Type Stars . He went on to receive his Diploma of Education at Christchurch Teachers College in New Zealand in November 1979 . He earned his Ph . D . in Geophysics in March 1985 from the Research School of Earth Sciences of the Australian National University, Canberra, Australia.
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