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VZ Cancri is a variable star in the constellationCancer, abbreviated VZ Cnc. It varies in brightness with a period of 0.178364 days, from an apparent visual magnitude of 7.18 down to 7.91, which lies below the typical threshold of visibility for the naked eye. The distance to this star is approximately 724 light years based on parallax measurements, and it is receding from the Sun with a radial velocity of 25 km/s.
This star was discovered to vary in brightness by B. S. Whitney in 1950, and was classified as a cluster-type Cepheid variable, or RR Lyrae star. In 1955, W. S. Fitch found the light curve to be variable and discovered a beat period of 0.716292 d, from which is inferred a second pulsation period of 0.1428041 days. H. A. Abt found that the stellar class of this star varied from A7–A9 III during peak brightness to F1–F2 III at minimum. After H. J. Smith pointed out the distinctiveness of short period RR Lyrae variables in 1956, VZ Cnc has been grouped under the category of Delta Scuti variables.
The star is located near the center of the instability strip. Both pulsation periods for this star are in the first and second overtone; it appears to lack a fundamental mode, possibly as a result of helium depletion in the outer atmosphere. In 1994, an examination of five decades of data on this star suggested a variation in the period of maximum light with a cycle length of 49.3 years. This could be the result of previously undetected pulsation frequencies.
^ Kahraman Aliçavuş, F.; et al. (October 2017), "High-resolution spectroscopy and abundance analysis of δ Scuti stars near the γ Doradus instability strip", Monthly Notices of the Royal Astronomical Society, 470 (4): 4408–4420, arXiv:1706.04782, Bibcode:2017MNRAS.470.4408K, doi:10.1093/mnras/stx1498.
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Abt, Helmut A. (November 1955), "Spectroscopic Observations of the Cluster-Type Variable VZ CANCRI.", Astrophysical Journal, 122: 390, Bibcode:1955ApJ...122..390A, doi:10.1086/146099.
^ Fu, J. -N.; Jiang, S. -Y. (April 1999), "Pulsation of the δ Scuti star VZ Cancri", Astronomy and Astrophysics Supplement, 136 (2): 285–292, Bibcode:1999A&AS..136..285F, doi:10.1051/aas:1999214.
Arellano Ferro, A.; Núñez, N. S.; Avila, J. J.; Trejoluna, J. J. (July 1994), "Period variations and duplicity of the δ Scuti star VZ Cancri", Revista Mexicana de Astronomía y Astrofísica, 29: 218, Bibcode:1994RMxAA..29..218A.
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Arellano Ferro, A.; et al. (June 1994), "Times of Light Maximum of VZ Cancri: 1994 Season", Information Bulletin on Variable Stars, 4039: 1, Bibcode:1994IBVS.4039....1A.
Quester, W. (June 1990), "Photoelectric Observations of VZ Cancri 1988-1990", Information Bulletin on Variable Stars, 3484: 1, Bibcode:1990IBVS.3484....1Q.
Garbuzov, G. A.; Mitskevich, A. S. (April 1984), "On the existence of an extended atmosphere in the delta Sct-type star VZ Cnc", Pis'ma v Astronomicheskii Zhurnal, 10: 223–228, Bibcode:1984PAZh...10..223G.
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Cester, B.; et al. (September 1977), "VZ Cancri", Information Bulletin on Variable Stars, 1338: 1, Bibcode:1977IBVS.1338....1C.
Todoran, I. (June 1976), "Photoelectric Maxima of VZ Cancri", Information Bulletin on Variable Stars, 1141: 1, Bibcode:1976IBVS.1141....1T.
Hahn, G.; et al. (December 1975), "Photoelectric Observations of VZ Cnc (HD 73857)", Information Bulletin on Variable Stars, 1078: 1, Bibcode:1975IBVS.1078....1H.
Catalano, C. P.; Neff, J. S. (1967), "Variations in the Photometric Properties of RR Lyrae and VZ Cancri with Beat Phase", Astronomical Journal, 72: 788, Bibcode:1967AJ.....72S.788C, doi:10.1086/110531.
Ponsen, J.; Oosterhoff, P. T. (1965), "Photoelectric observations of VZ Cnc and RZ Cep", Bulletin of the Astronomical Institutes of the Netherlands, 18: 459, Bibcode:1965BAN....18..459P.