Advertisement

Interstellar Matter

  • Yoshiaki Sofue
Chapter
Part of the Lecture Notes in Physics book series (LNP, volume 935)

Abstract

Interstellar space is filled with interstellar matter (ISM) composed of various kinds of gases from low temperature (molecules, HI gas, and dust) to high temperature (ionized gas, HII regions), high-energy particles (cosmic rays), and magnetic fields. They are embedded in the radiation field of stars. The ISM makes up approximately 10% of the mass of the galactic disk, and the majority is HI and H2. The remaining 90% is shared by stars and dark matter, which determine the dynamical properties of the galaxy. The IMS is deeply coupled to activities such as the star formation near the galactic plane, and is categorized as younger-generation matter in the galaxy, called Population I.

Keywords

Star Formation Brightness Temperature Molecular Cloud Column Density Galactic Plane 
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.

References

  1. 1.
    Bolatto, A.D., Wolfire, M., Leroy, A.K.: The CO-to-H2 conversion factor. ARAA 51, 207 (2013). [CO to H2 conversion factor]Google Scholar
  2. 2.
    Dickey, J.M., Lockman, F.J.: HI in the galaxy. ARAA 28, 215 (1990). [HI gas in the Galaxy]Google Scholar
  3. 3.
    Dickman, R.L., Snell, J.S., Young, J.S. (eds.): Molecular Clouds in the Milky Way and External Galaxies. Springer, Berlin/New York (1988). [HI gas in the Galaxy]Google Scholar
  4. 4.
    Elmegreen, B.G.: The H to H2 transition in galaxies – totally molecular galaxies. ApJ 411, 170 (1993). [HI-H2 transfer]Google Scholar
  5. 5.
    Haynes, M.P., Giovanelli, R., Chincarini, G.L.: The influence of environment on the HI content of galaxies. ARAA 22, 445 (1984). [HI in galaxies]Google Scholar
  6. 6.
    Kaplan, S.A., Pikel’ner, S.B.: Large-scale dynamics of the interstellar medium. ARAA 12, 113 (1974). [ISM; review]Google Scholar
  7. 7.
    Maloney, P., Black, J.H.: I(CO)∕N(H2) conversions and molecular gas abundances in spiral and irregular galaxies. ApJ 325, 389 (1988). [CO-H2 Converson factor]Google Scholar
  8. 8.
    Nakai, N., Kuno, N., Handa, T., Sofue, Y.:. Distribution and dynamics of molecular gas in the galaxy M51. 1: data and spiral structure. PASJ 46, 527 (1994). [CO in M51]Google Scholar
  9. 9.
    Rots, A.H., Bosma, A., van der Hulst, J.M., Athanassoula, E., Crane, P.C.: High-resolution HI observations of the Whirlpool Galaxy M51. AJ 100, 387 (1990). [HI in M51]Google Scholar
  10. 10.
    Shull, J.M., Beckwith, S.: Interstellar molecular hydrogen. ARAA 20, 163 (1982). [Molecular gas, review]Google Scholar
  11. 11.
    Spitzer, L.: Physical Processes in the Interstellar Medium. Wiley, San Fransisco (1978). [ISM; text book]Google Scholar
  12. 12.
    Young, J.S., Scoville, N.Z.: Molecular gas in galaxies. ARA&A 29, 581 (1991) [CO in galaxies, review]Google Scholar

Copyright information

© Springer Nature Singapore Pte Ltd. 2017

Authors and Affiliations

  • Yoshiaki Sofue
    • 1
  1. 1.Institute of AstronomyThe University of TokyoMitakaJapan

Personalised recommendations