A Spectroscopic Orbit for the Late-type Be Star beta CMi

作者：Dulaney Nicholas A; Richardson Noel D^*; Gerhartz Cody J; Bjorkman J E; Bjorkman K S; Carciofi Alex C; Klement Robert; Wang Luqian; Morrison Nancy D; Bratcher Allison D; Greco Jennifer J; Hardegree Ullman Kevin K; Lembryk Ludwik; Oswald Wayne L; Trucks Jesica L

来源：Astrophysical Journal, 2017, 836(1): 112.

DOI：10.3847/1538-4357/836/1/112

• binaries: spectroscopic
• stars: emission-line, Be
• stars: individual (beta CMi)

The late-type Be star beta CMi is remarkably stable compared to other Be stars that have been studied. This has led to a realistic model of the outflowing Be disk by Klement et al. These results showed that the disk is likely truncated at a finite radius from the star, which Klement et al. suggest is evidence for an unseen binary companion in orbit. Here we report on an analysis of the Ritter Observatory spectroscopic archive of a CMi to search for evidence of the elusive companion. We detect periodic Doppler shifts in the wings of the Ha line with a period of 170 days and an amplitude of 2.25 km s(-1) , consistent with a low-mass binary companion (M approximate to 0.42M circle dot). We then compared small changes in the violet-to-red peak height changes (V/R) with the orbital motion. We find weak evidence that it does follow the orbital motion, as suggested by recent Be binary models by Panoglou et al. Our results, which are similar to those for several other Be stars, suggest that beta CMi may be a product of binary evolution where Roche lobe overflow has spun up the current Be star, likely leaving a hot subdwarf or white dwarf in orbit around the star. Unfortunately, no direct sign of this companion star is found in the very limited archive of International Ultraviolet Explorer spectra.

• 出版日期2017-2-10