Universität zu Köln

Kaminski, T., Mueller, H. S. P., Schmidt, M. R., Cherchneff, I., Wong, K. T., Bruenken, S., Menten, K. M., Winters, J. M., Gottlieb, C. A. and Patel, N. A. (2017). An observational study of dust nucleation in Mira (o Ceti) II. Titanium oxides are negligible for nucleation at high temperatures. Astron. Astrophys., 599. LES ULIS CEDEX A: EDP SCIENCES S A. ISSN 1432-0746

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Abstract

Context. The formation of silicate dust in oxygen-rich envelopes of evolved stars is thought to be initiated by the formation of seed particles that can withstand the high temperatures close to the stellar photosphere and act as condensation cores farther away from the star. TiO and TiO2 are among the candidate species considered as first condensates. Aims. We aim to identify and characterize the circumstellar gas-phase chemistry of titanium that leads to the formation of solid titanium compounds in the envelope of o Ceti, the prototypical Mira, and seek an observational verification of whether titanium oxides play a major role in the onset of dust formation in M-type asymptotic giant branch (AGB) stars. Methods. We present high angular resolution (145 mas) ALMA observations at submillimeter (submm) wavelengths supplemented by APEX and Herschel spectra of the rotational features of TiO and TiO2. In addition, circumstellar features of TiO and Ti i are identified in optical spectra, which cover multiple pulsation cycles of o Ceti. Results. The submm ALMA data reveal TiO and TiO2 bearing gas within the extended atmosphere of Mira. While TiO is traceable up to a radius (FWHM/2) of 4.0 stellar radii (R-star), TiO2 extends as far as 5.5 R-star and, unlike TiO, appears to be anisotropically distributed. Optical spectra display variable emission of Ti I and TiO from inner parts of the extended atmosphere (< 3 R-star). Conclusions. Chemical models that include shocks are in general agreement with the observations of gas-phase, titanium-bearing molecules. It is unlikely that substantial amounts of titanium is locked up in solids because the abundance of the gaseous titanium species is very high. The formation of hot titanium-rich condensates is very improbable because we find no traces of their hot precursor species in the gas phase. It therefore appears unlikely that the formation of dust in Mira, and possibly other M-type AGB stars, is initiated by titanium oxides.

Item Type:	Journal Article
Creators:	Creators Email ORCID ORCID Put Code Kaminski, T. UNSPECIFIED UNSPECIFIED UNSPECIFIED Mueller, H. S. P. UNSPECIFIED UNSPECIFIED UNSPECIFIED Schmidt, M. R. UNSPECIFIED UNSPECIFIED UNSPECIFIED Cherchneff, I. UNSPECIFIED UNSPECIFIED UNSPECIFIED Wong, K. T. UNSPECIFIED UNSPECIFIED UNSPECIFIED Bruenken, S. UNSPECIFIED UNSPECIFIED UNSPECIFIED Menten, K. M. UNSPECIFIED UNSPECIFIED UNSPECIFIED Winters, J. M. UNSPECIFIED UNSPECIFIED UNSPECIFIED Gottlieb, C. A. UNSPECIFIED UNSPECIFIED UNSPECIFIED Patel, N. A. UNSPECIFIED UNSPECIFIED UNSPECIFIED
URN:	urn:nbn:de:hbz:38-237936
DOI:	10.1051/0004-6361/201629838
Journal or Publication Title:	Astron. Astrophys.
Volume:	599
Date:	2017
Publisher:	EDP SCIENCES S A
Place of Publication:	LES ULIS CEDEX A
ISSN:	1432-0746
Language:	English
Faculty:	Unspecified
Divisions:	Unspecified
Subjects:	no entry
Uncontrolled Keywords:	Keywords Language SHOCK-INDUCED VARIABILITY; PURE ROTATIONAL SPECTRUM; EMISSION-LINES; INNER WIND; MOLECULAR-SPECTROSCOPY; INFRARED-SPECTROSCOPY; RADIO PHOTOSPHERES; COLOGNE DATABASE; SILICATE DUST; RICH Multiple languages Astronomy & Astrophysics Multiple languages
Refereed:	Yes
URI:	http://kups.ub.uni-koeln.de/id/eprint/23793