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On producers of cosmic organic compounds: exploring the boron abundance in lithium-rich K giant stars

Published online by Cambridge University Press:  04 September 2018

N. A. Drake ,
R. de la Reza ,
V. V. Smith  and
K. Cunha
N. A. Drake
Affiliation:
Observatório Nacional-MCTIC, Rua Gen. José Cristino 77, 20921-400, Rio de Janeiro, Brazil, email: [email protected], [email protected], [email protected] St. Petersburg State University, Laboratory of Observational Astrophysics, Universitetski pr. 28, 198504, St. Petersburg, Russia
R. de la Reza
Affiliation:
Observatório Nacional-MCTIC, Rua Gen. José Cristino 77, 20921-400, Rio de Janeiro, Brazil, email: [email protected], [email protected], [email protected]
V. V. Smith
Affiliation:
National Optical Astronomy Observatory, 950 North Cherry Ave., Tucson, AZ 85719, USA, email: [email protected], [email protected]
K. Cunha
Affiliation:
Observatório Nacional-MCTIC, Rua Gen. José Cristino 77, 20921-400, Rio de Janeiro, Brazil, email: [email protected], [email protected], [email protected] National Optical Astronomy Observatory, 950 North Cherry Ave., Tucson, AZ 85719, USA, email: [email protected], [email protected]
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Abstract

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The element boron belongs, together with lithium and beryllium, to a known trio of important elements for the study of evolutionary processes in low mass stars. Because B is the least fragile of this trio to be destroyed in the stellar interiors, it can be used to test if the Li enrichment is of planetary origin. Here, for the first time, boron lines are examined in the UV for four giants with different degrees of large Li enrichment by means of observations with the Hubble telescope. Two main results are found in our study. One is that to first approximation B abundances appear not to be in excess, invalidating the planet engulfment mechanism. The second one is that the two stars with very large Li abundances present emission lines indicating that quite strong active chromospheres are acting in these very Li-rich giants. These new results obtained from the UV complement our recent studies in the mid-IR (de la Reza et al. 2015) where strong emission-line features of organic material were found in the spectra of some Li-rich stars.

Keywords

stars: abundances – stars: chemically peculiar – stars: magnetic field – stars: mass loss – stars: individual: HD 787HD 9746HD 39853HD 112127
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 13 , Symposium S332: Astrochemistry VII: Through the Cosmos from Galaxies to Planets , March 2017 , pp. 237 - 241
Copyright
Copyright © International Astronomical Union 2018 

References

Aurière, M., Konstantinova-Antova, R., Charbonnel, C., et al. 2015, A&A, 574, A90Google Scholar
Balachandran, S. C., Fekel, F. C., Henry, G. W., & Uitenbroek, H. 2000, ApJ, 542, 978Google Scholar
Brown, J. A., Sneden, C., Lambert, D. L., & Dutchover, E. 1989, ApJS, 71, 293Google Scholar
Castilho, B. V., Spite, F., Barbuy, B. et al,. 1999, A&A, 345 249Google Scholar
Cunha, K., Smith, V. V., Boesgaard, A. M., & Lambert, D. L. 2000, ApJ, 530, 939Google Scholar
de la Reza, R., Drake, N. A., Oliveira, I., & Rengaswamy, S. 2015, ApJ, 806, 86Google Scholar
Drake, N. A., de~la~Reza, R., da~Silva, L., & Lambert, D. L. 2002, AJ, 123, 2703Google Scholar
Duncan, D. K., Peterson, R. C., Thorburn, J. A., & Pinsonneault, M. H. 1998, ApJ, 499, 871Google Scholar
Eggleton, P. & Tokovinin, A. 2008, MNRAS, 389, 869Google Scholar
Fekel, F. C. & Balachandran, S. 1993, ApJ, 403, 708Google Scholar
Goriely, S. 2007, A&A, 466, 619Google Scholar
Gratton, R. G. & D’Antona, F. 1989, A&A, 215, 66Google Scholar
Johansson, S. & Hamann, F. 1993, Phys. Scr., T47, 157Google Scholar
Lebouteiller, V., Barry, D. J., Spoon, H. W. W., et al. 2011, ApJS, 196, 8Google Scholar
Mason, B. D., Martin, C., Hartkopf, W. I., et al. 1999, AJ, 117, 1890Google Scholar
Melo, C. H. F., de Laverny, P., Santos, N. C., et al. 2005, A&A, 439, 227Google Scholar
Privitera, G., Meynet, G., Eggenberger, P., et al. 2016, A&A, 593, L15Google Scholar
Sneden, C. 1973, PhD Thesis, Univ. of Texas at AustinGoogle Scholar
Wallerstein, G. & Sneden, C. 1982, ApJ, 255, 577Google Scholar