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[en] It is widely accepted that pulsating variables with periods less than 0.2 day fall into two distinct groups: RR type stars and delta Scuti type stars. The physical properties of these groups are examined to see whether any clear-cut difference can be found. It is suggested that the two groups are fundamentally similar: hydrogen shell burning stars of about two solar masses. The only difference is the mode of pulsation. (P.J.S.)
Source
Sherwood, V.E.; Plaut, L. (eds.); International Astronomical Union; p. 243-246; ISBN 902770578X; 
; 1975; D. Reidel; Dordrecht, The Netherlands; Variable stars and stellar evolution; Moscow, USSR; 29 Jul 1974
; 1975; D. Reidel; Dordrecht, The Netherlands; Variable stars and stellar evolution; Moscow, USSR; 29 Jul 1974
No abstract available
Source
Mueller, E.A.; International Astronomical Union; p. 27-28; ISBN 90-277-0850-9; ; 1977; p. 27-28; D. Reidel; Dordrecht, Netherlands; 16. general assembly of the International Astronomical Union; Grenoble, France; Aug 1976; Published in summary form pnly.
; 1977; p. 27-28; D. Reidel; Dordrecht, Netherlands; 16. general assembly of the International Astronomical Union; Grenoble, France; Aug 1976; Published in summary form pnly.
No abstract available
Journal
Nature (London); ISSN 0028-0836; ; v. 283(5742); p. 50-51
; v. 283(5742); p. 50-51
[en] A narrow-band photometric system is described which differentiates stars on the lower main sequence from giants. 1251 stars have been observed on this system and 90 of these shown to be dwarfs, apart from those dwarfs used to calibrate the system. (author)
Journal
Monthly Notices of the Royal Astronomical Society; ISSN 0035-8711; ; v. 194(2); p. 403-419
; v. 194(2); p. 403-419
[en] The light curve of the Crab Nebula pulsar has been observed using an aperture of 1.3 arcsec with the Anglo-Australian Telescope. The background was measured in an annulus of 2 arcsec radius, contamination from the pulsar being estimated from the pulsed component. The resultant light curve has a minimum intensity 0.6 per cent of the peak. Around minimum the light is approximately 70 per cent linearly polarized, and at other phases our measures accord with earlier work. (author)
Journal
Monthly Notices of the Royal Astronomical Society; ISSN 0035-8711; ; v. 196(3); p. 943-953
; v. 196(3); p. 943-953
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