An observational study of dust nucleation in Mira (o Ceti)
II. Titanium oxides are negligible for nucleation at high temperatures
1 ESO, Alonso de Cordova 3107, Vitacura, 19001 Casilla, Santiago, Chile
2 Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA, USA
3 I. Physikalisches Institut, Universität zu Köln, Zülpicher Strasse 77, 50937 Köln, Germany
4 Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences, Rabiańska 8, 87-100 Toruń, Poland
5 Departement Physik, Universität Basel, Klingelbergstrasse 82, 4056 Basel, Switzerland
6 Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany
7 IRAM, 300 rue de la Piscine, Domaine Universitaire de Grenoble, 38406 St.-Martin-d’ Hères, France
Received: 4 October 2016
Accepted: 9 November 2016
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⋆), TiO2 extends as far as 5.5 R⋆ 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⋆).
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.
Key words: stars: mass-loss / circumstellar matter / astrochemistry / stars: individual: o Ceti / submillimeter: stars
© ESO, 2017