The Maser-emitting Structure and Time Variability of the SiS Lines J = 14-13 and 15-14 in IRC+10216
| Autor: | C. Sánchez Contreras, Marcelino Agúndez, A. Castro-Carrizo, José Pablo Fonfría, José Cernicharo, M. Santander-García, Juan R. Pardo, G. Quintana-Lacaci, Manuel Fernández-López, L. Velilla-Prieto, Salvador Curiel |
|---|---|
| Přispěvatelé: | Universidad Nacional Autónoma de México, Ministerio de Economía y Competitividad (España), European Commission |
| Rok vydání: | 2018 |
| Předmět: |
010504 meteorology & atmospheric sciences
Ciencias Físicas oscillations [Stars] Line: profiles (Stars:) circumstellar matter FOS: Physical sciences individual (IRC+10216) [Stars] Astrophysics::Cosmology and Extragalactic Astrophysics Astrophysics Stars: individual (IRC+10216) 01 natural sciences ) circumstellar matter [(Stars] law.invention purl.org/becyt/ford/1 [https] Techniques: high angular resolution Telescope law Stars: oscillations 0103 physical sciences Radiative transfer Astrophysics::Solar and Stellar Astrophysics Angular resolution Masers Maser 010303 astronomy & astrophysics Solar and Stellar Astrophysics (astro-ph.SR) Astrophysics::Galaxy Astrophysics 0105 earth and related environmental sciences Physics Stars: AGB and post-AGB Astronomy and Astrophysics purl.org/becyt/ford/1.3 [https] Thermal emission AGB and post-AGB [Stars] Circumstellar matter Astronomía profiles [Line] high angular resolution [Techniques] Interferometry Astrophysics - Solar and Stellar Astrophysics 13. Climate action Space and Planetary Science Excited state Techniques: interferometric interferometric [Techniques] CIENCIAS NATURALES Y EXACTAS Stellar pulsation |
| Zdroj: | Digital.CSIC. Repositorio Institucional del CSIC instname CONICET Digital (CONICET) Consejo Nacional de Investigaciones Científicas y Técnicas instacron:CONICET |
| ISSN: | 2009-0730 |
| Popis: | 18 pags., 11 figs., 3 tabs., 2 apps. We present new high angular resolution interferometer observations of the v = 0 J = 14-13 and 15-14 SiS lines toward IRC+10216, carried out with the Combined Array for Research in Millimeter-wave Astronomy and the Atacama Large Millimeter Array. The maps, with angular resolutions of ≃0.″25 and 0.″55, reveal (1) an extended, roughly uniform, and weak emission with a size of ≃0.″5; (2) a component elongated approximately along the east-west direction peaking at ≃0.″13 and 0.″17 at both sides of the central star; and (3) two blue- and redshifted compact components peaking around 0.″07 to the NW of the star. We have modeled the emission with a 3D radiation transfer code, finding that the observations cannot be explained only by thermal emission. Several maser clumps and one arc-shaped maser feature arranged from 5 to 20 from the central star, in addition to a thin shell-like maser structure at ≃13 , are required to explain the observations. This maser-emitting set of structures accounts for 75% of the total emission, while the other 25% is produced by thermally excited molecules. About 60% of the maser emission comes from the extended emission, and the rest comes from the set of clumps and the arc. The analysis of a time monitoring of these and other SiS and SiS lines carried out with the IRAM 30 m telescope from 2015 to present suggests that the intensity of some spectral components of the maser emission strongly depends on the stellar pulsation, while other components show a mild variability. This monitoring evidences a significant phase lag of ≃0.2 between the maser and near-IR light curves. During the first part of this work, J.P.F. was supported by the UNAM through a postdoctoral fellowship. J.C., M.A., L.V.P., G.Q.-L., M.S.-G., J.R.P., and J.P.F. thank the Spanish MINECO/MICINN for funding support through grants AYA2009-07304, AYA2012-32032, AYA2016-75066-C-1-P, the ASTROMOL Consolider project CSD2009-00038, and the European Research Council (ERC Grant 610256: NANOCOSMOS). M.A. also acknowledges funding support from the Ramón y Cajal program of Spanish MINECO (RyC-2014- 16277). |
| Databáze: | OpenAIRE |
| Externí odkaz: |
|