Silicon isotopic abundance toward evolved stars and its application for presolar grains^⋆,⋆⋆

¹ ESO Garching, Karl-Schwarzschild Str. 2 85748 Garching, Germany
e-mail: tpeng@eso.org
² Excellence Cluster Universe, Boltzmannstr. 2, 85748 Garching, Germany
³ INAF – Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 50125 Firenze, Italy
⁴ Univ. Bordeaux, LAB, UMR 5804, 33270 Floirac, France
⁵ CNRS, LAB, UMR 5804, 33270 Floirac, France
⁶ National Radio Astronomy Observatory, 520 Edgemont Road, Charlottesville, VA 22903, USA
⁷ Department of Earth and Space Sciences, Chalmers University of Technology, Onsala Space Observatory, 439 92 Onsala, Sweden
⁸ Joint ALMA Observatory (JAO) and European Southern Observatory, Alonso de Córdova 3107, Vitacura, Santiago, Chile
⁹ JBCA, Alan Turing Building, School of Physics and Astronomy, University of Manchester, Manchester M13 9PL, UK

Received: 9 August 2013
Accepted: 18 October 2013

Abstract

Aims. Galactic chemical evolution (GCE) is important for understanding the composition of the present-day interstellar medium (ISM) and of our solar system. In this paper, we aim to track the GCE by using the ²⁹Si/³⁰Si ratios in evolved stars and tentatively relate this to presolar grain composition.

Methods. We used the APEX telescope to detect thermal SiO isotopologue emission toward four oxygen-rich M-type stars. Together with the data retrieved from the Herschel science archive and from the literature, we were able to obtain the ²⁹Si/³⁰Si ratios for a total of 15 evolved stars inferred from their optically thin ²⁹SiO and ³⁰SiO emission. These stars cover a range of masses and ages, and because they do not significantly alter ²⁹Si/³⁰Si during their lifetimes, they provide excellent probes of the ISM metallicity (or ²⁹Si/³⁰Si ratio) as a function of time.

Results. The ²⁹Si/³⁰Si ratios inferred from the thermal SiO emission tend to be lower toward low-mass oxygen-rich stars (e.g., down to about unity for W Hya), and close to an interstellar or solar value of 1.5 for the higher-mass carbon star IRC+10216 and two red supergiants. There is a tentative correlation between the ²⁹Si/³⁰Si ratios and the mass-loss rates of evolved stars, where we take the mass-loss rate as a proxy for the initial stellar mass or current stellar age. This is consistent with the different abundance ratios found in presolar grains. Before the formation of the Sun, the presolar grains indicate that the bulk of presolar grains already had ²⁹Si/³⁰Si ratios of about 1.5, which is also the ratio we found for the objects younger than the Sun, such as VY CMa and IRC+10216. However, we found that older objects (up to possibly 10 Gyr old) in our sample trace a previous, lower ²⁹Si/³⁰Si value of about 1. Material with this isotopic ratio is present in two subclasses of presolar grains, providing independent evidence of the lower ratio. Therefore, the ²⁹Si/³⁰Si ratio derived from the SiO emission of evolved stars is a useful diagnostic tool for the study of the GCE and presolar grains.