Prog. Theor. Phys. Vol. 24 No. 5 (1960) pp. 1131-1132
Possible Methods for Detecting Intergalactic Hydrogen
Physical Institute, Nagoya University, Nagoya
(Received August 29, 1960)
DOI : 10.1143/PTP.24.1131
See, for example, F. D. Kahn and L. Woltjer, Astrophys. J. 130 (1959), 705[CrossRef].
- L. Spitzer and J. L. Greenstein, Astrophys. J. 104 (1951), 407,
have suggested the importance of this process in connection with the luminosity of a planetary nebula.
The author is grateful to Professor W. Unno who called his attention to the above paper and stimulated him by suggestive comments.
- This process is regarded as the most important cause of the ultraviolet radiation from Galactic clouds, as was discussed by the author.
S. Hayakawa, Publ. Astron. Soc. Jpn. 12 (1960), 110; ibid. 12 (1960), 113.
- This and related processes are analyzed in more detail and are applied to the ultraviolet radiation from Galactic clouds.
The work will soon be published by S. Hayakawa, S. Nishimura and K. Takayanagi.
See, for example, J. E. Kupperian, Jr, A. Bogges III and J. E. Milligan, Astrophys. J. 128 (1958), 453[CrossRef].
- P. Morrison, Nuovo Cim. Suppl. 8 (1958), 858.