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Cosmic Rays from Regions of Star Formation I. The Carina Complex

Published online by Cambridge University Press:  14 August 2015

T. Montmerle ,
J. A. Paul  and
M. Cassé
T. Montmerle
Affiliation:
Section d'Astrophysique Centre d'Etudes Nucléaires de Saclay, France
J. A. Paul
Affiliation:
Section d'Astrophysique Centre d'Etudes Nucléaires de Saclay, France
M. Cassé
Affiliation:
Section d'Astrophysique Centre d'Etudes Nucléaires de Saclay, France

Extract

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Within the error circle of the COS-B gamma-ray source at ℓ = 288°, b = 0° lies the Carina Nebula, one of the most active regions of star formation known, housing several OB associations and Wolf-Rayet stars (WRS), and perhaps also a supernova remnant (SNR). As a region containing intense mass-losing stars it belongs to the same species as the Rho Oph cloud (but much more active), suggested to be associated with the gamma-ray source at ℓ = 353°, b = +16° (Paul et al., this conference). As a group of OB association linked with a SNR, it belongs to the same species as “SNOB's” (Montmerle, 1979), possibly identified with about half of the COS-B sources. We suggest that the source at ℓ = 288°, b = 0° should be identified with the Carina complex. In this case the source would be at ≃ 2.7 kpc and its gamma-ray luminosity would be ≃ 2.1035 erg s−1. It is suggestive that the nearest aggregate of stars, gas and dust (Rho Oph) and the richest one (Carina) are both in the direction of a gamma-ray source. The Carina complex is noted in particular for the compact star clusters Tr 14, Tr 16 and Cr 228 (Humphreys, 1978), altogether comprising 6 of the 7 O3 stars observed in the Galaxy. It is also remarkable that 3 WRS are associated with the complex. All 3 WRS are of the WN7 type, having the highest mass-loss rate of WRS (≃ 10−4 M⊙ yr−1). Even more remarkable is the presence of the strange Carina object which sheds mass at the extraordinary rate of 10−3 to 0.075 M⊙ yr−1, with a velocity of ≃ 600 km s−1. Moreover, according to radio (Jones, 1973) and optical (Elliot, 1979) data, there seems to be a SNR buried in the Nebula. However, it is not seen at X-ray wavelengths by the Einstein observatory (Seward et al., 1979). This could be explained if the SNR has a luminosity Lx < 1034 erg s−1, since it could then be conceivably hidden by the unstructured, diffuse X-background. The molecular cloud associated with the Carina Nebula has been observed in the lines of H2CO and OH (Dickel, 1974). The cloud has a derived mass of ≲ 105 M⊙, typical of other molecular clouds.

Type
Research Article
Information
Symposium - International Astronomical Union , Volume 94: Origin of Cosmic Rays , 1981 , pp. 321 - 322
Copyright
Copyright © Reidel 1981 

References

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