Radio Emission from Novae and Supernovae

Attempts have been made to observe the radio emission at 3?5 m from two supernovae and ten novae. Kepler's star was the only reasonably certain identification. A comparison with radio observations of other supernova remnants suggests a constant ratio between the present radio emission and the maximum emission of light. It is concluded that for common novae, which are not detectable as radio sources, this ratio must be smaller than for supernovae. The galactic radio emission near the plane of the Milky Way could be largely the integrated emission of supernova remnants but common novae could not contribute appreciably.

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Some Observations of Shell-type Galactic Radio Sources

Australian Journal of Physics ◽

10.1071/ph670297 ◽

1967 ◽

Vol 20 (3) ◽

pp. 297 ◽

Cited By ~ 12

Author(s):

ER Hill

Keyword(s):

Radio Emission ◽

Spherical Symmetry ◽

Supernova Remnants ◽

Supernova Remnant ◽

Milky Way ◽

Radio Sources ◽

Radio Observations ◽

Shell Type ◽

Rosette Nebula ◽

Galactic Radio

Radio evidence for two new supernova remnants in the Southern Milky Way is presented. Some new observations of the known supernova remnant, source 1439-62, and of the Rosette nebula, a shell source but not a supernova remnant, are also presented. The problem of finding model shells to fit the radio observations is considered and it is shown that the radio emission from 1439-62 is unlikely to originate in a shell with spherical symmetry.

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Extended Radio Sources. II.

Australian Journal of Physics ◽

10.1071/ph650077 ◽

1965 ◽

Vol 18 (1) ◽

pp. 77 ◽

Cited By ~ 2

Author(s):

PAG Scheuer

Keyword(s):

Radio Emission ◽

Angular Diameter ◽

Radio Sources ◽

Extended Source ◽

Previous Communication ◽

Extended Radio ◽

Galactic Radio Emission ◽

Galactic Radio

Detailed observations of "extended radio sources" were reported in a previous communication. Some of these sources are probably irregularities in the galactic radio emission, but at high galactic latitudes the typical extended source consists of a group of sources of small angular diameter.

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Extended Radio Sources. I.

Australian Journal of Physics ◽

10.1071/ph640106 ◽

1964 ◽

Vol 17 (1) ◽

pp. 106 ◽

Cited By ~ 4

Author(s):

DK Milne ◽

PAG Scheuer

Keyword(s):

Radio Emission ◽

Principal Component ◽

Angular Diameter ◽

Radio Sources ◽

Pencil Beam ◽

Optical Identification ◽

Extended Radio ◽

Extended Sources ◽

Galactic Radio Emission ◽

Galactic Radio

Twenty�one "extended sources" from the catalogues of Mills, Slee, and Hill have been observed with a 14' arc pencil beam at 1400 Mc/s. Some appear to be irregularities in the galactic radio emission, but most, especially those at high galactic latitudes, are resolved into groups of sources of small angular diameter. Maps of the regions are shown, and so far as possible radio spectra of the component sources have been assembled. An optical identification is given for the principal component of MSH 00-017 (3C29), and tentative identifications are suggested for some other sources.

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Some new observations relating to galactic radio sources and background structure

Symposium - International Astronomical Union ◽

10.1017/s0074180900052372 ◽

1964 ◽

Vol 20 ◽

pp. 107-114 ◽

Cited By ~ 1

Author(s):

E. R. Hill

Keyword(s):

Radio Emission ◽

Radio Telescope ◽

Milky Way ◽

Angular Resolution ◽

Spectral Information ◽

Radio Sources ◽

Background Structure ◽

The Galaxy ◽

Galactic Radio

A survey of the distribution of radio emission at wavelengths of 75 and 20 cm along an extensive section of the Southern Milky Way has recently been carried out by M. Komesaroff and myself using the 210-foot radio telescope at Parkes. The area surveyed ranges from lII = 280 to 355° and extends on the average to 6 degrees either side of the plane. The beamwidths of the aerial at 75 and 20 cm are 50 and 14 min arc respectively. Observations at the shorter wavelength offer a picture of this section of the Galaxy at considerably higher angular resolution than hitherto available, while the 75-cm observations are expected to make a useful contribution to our spectral information.

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