A light curve for IQ Aurigae from BRITEnanosatellites. Plotted from data published by Strassmeier et al. (2020),[11] assuming a period of 2.463 days.
In 1953, Sanford S Provin reported that the star, referred to at that time as HD 34452, showed indications of being a variable star, but the evidence was inconclusive.[12] Karl D. Rakos confirmed that the star is variable in 1962.[13]
This is a magnetic Ap star with a stellar classification of A0pSi.[3] It is known as a silicon star, having a strong line of singly ionized silicon, and may also be helium deficient as the lines of helium are weaker than expected.[9] The star is an Alpha2 Canum Venaticorum-type variable, ranging in magnitude from 5.35 down to 5.43 with a rotationally-modulated period of 2.4660days.[6] It is an X-ray source with a high luminosity of 4×1029erg s−1, which may be caused by a combination of shocks in the stellar wind and magnetic reconnection occurring well above the stellar surface. The star has been observed to flare, during which the X-ray emission rose to 3.2×1031erg s−1.[3]
↑Cowley, A.; etal. (April 1969), "A study of the bright A stars. I. A catalogue of spectral classifications", Astronomical Journal, 74: 375–406, Bibcode:1969AJ.....74..375C, doi:10.1086/110819.
↑Mermilliod, J.-C. (1986), "Compilation of Eggen's UBV data, transformed to UBV (unpublished)", Catalogue of Eggen's UBV Data. SIMBAD, Bibcode:1986EgUBV........0M.
12Tomley, L. J.; etal. (December 1970), "A spectroscopic analysis of the silicon star HD 34452.", Astronomy and Astrophysics, 9: 380–391, Bibcode:1970A&A.....9..380T.
