What causes long secondary periods in ~25% of AGB stars?

Details What causes long secondary periods in ~25% of AGB stars? What causes long secondary periods in ~25% of AGB stars?

Feb 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005noao.prop...96w&link_type=abstract

NOAO Proposal ID #2005A-0096

Computer Science

Scientific paper

About 25% of variable asymptotic giant branch stars in the LMC have light curves that are modulated by a long secondary period (LSP) of length ~1-4 years. Solar-vicinity analogs of these stars show radial velocity curves that are asymmetric and of small amplitude (~3-5 km s^-1). Possible explanations for the photometric and radial velocity variations include eccentric motion of an orbiting companion of mass ~0.1 M_&sun;, radial and nonradial pulsation, rotation of an ellipsoidal-shaped red giant, episodic dust ejection, and star spot cycles. However, there are severe difficulties with each of these models. Thus the LSPs are the only unexplained type of large- amplitude stellar variability known at this time. In this study, we will examine simultaneous photometric and radial velocity variations in a large sample of LMC variables having a range of periods and photometric amplitudes in an attempt to discover the origin of the LSPs.

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