X Herculis and TX Piscium: two cases of ISM interaction with stellar winds observed by<i>Herschel</i>

Jorissen, A.; Mayer, Andreas; Eck, S. Van; Ottensamer, R.; Kerschbaum, F.; Ueta, Toshiya; Bergman, P.; Blommaert, J. A. D. L.; Decin, L.; Groenewegen, M. A. T.; Hron, J.; Nowotny, W.; Olofsson, H.; Posch, Th.; Sjouwerman, Loránt O.; Vandenbussche, B.; Waelkens, Christoffel

doi:10.1051/0004-6361/201116927

Cited by 27 publications

(47 citation statements)

References 79 publications

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“…A deviation from spherical symmetry for the circumstellar environment of TX Psc was detected by several authors at different spatial scales and wavelengths (e.g. Cruzalèbes et al 1998;Ragland et al 2006;Sacuto et al 2011b;Jorissen et al 2011;Hron et al, in prep.). Clearly, the circumstellar environment of TX Psc is very complex, and most likely unrelated effects shape the morphology in different regions, resulting in a wide variety of structures.…”

Section: Approach 1: Geometric Modelsmentioning

confidence: 85%

“…TX Psc is one of the brightest and closest carbon-rich AGB stars. It is listed as an irregular variable in the General Catalogue of Variable stars (Samus et al 2009) with a mean brightness of ∼5 mag and a peak-to-peak amplitude of 0.4 mag in the V-band (Jorissen et al 2011). Distance estimates range from 275 to 315 pc (van Leeuwen 2007;Claussen et al 1987;Bergeat & Chevallier 2005).…”

Section: Introductionmentioning

confidence: 99%

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Catching the fish – Constraining stellar parameters for TX Piscium using spectro-interferometric observations

Klotz

Paladini

Hron

et al. 2013

A&A

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Context. Stellar parameter determination is a challenging task when dealing with galactic giant stars. The combination of different investigation techniques has proven to be a promising approach. Aims. We analyse archive spectra obtained with the Short Wavelength Spectrometer (SWS) onboard ISO, and new interferometric observations from the Very Large Telescope MID-infrared Interferometric instrument (VLTI/MIDI) of a very well studied carbon-rich giant: TX Psc. The aim of this work is to determine stellar parameters using spectroscopy and interferometry. Methods. The observations are used to constrain the model atmosphere, and eventually the stellar evolutionary model in the region where the tracks map the beginning of the carbon star sequence. Two different approaches are used to determine stellar parameters: (i) the "classic" interferometric approach where the effective temperature is fixed by using the angular diameter in the N-band (from interferometry) and the apparent bolometric magnitude; (ii) parameters are obtained by fitting a grid of state-of-the-art hydrostatic models to spectroscopic and interferometric observations. Results. We find good agreement between the parameters of the two methods. The effective temperature and luminosity clearly place TX Psc in the carbon-rich AGB star domain in the H-R-diagram. Current evolutionary tracks suggest that TX Psc became a C-star just recently, which means that the star is still in a "quiet" phase compared to the subsequent strong-wind regime. This agrees with the C/O ratio being only slightly greater than one.

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Section: Approach 1: Geometric Modelsmentioning

confidence: 85%

Section: Introductionmentioning

confidence: 99%

Catching the fish – Constraining stellar parameters for TX Piscium using spectro-interferometric observations

Klotz

Paladini

Hron

et al. 2013

A&A

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“…An overview of the MESS objects is given by Cox et al (2012) and detailed studies of individual objects are presented in Ladjal et al (2010a), Kerschbaum et al (2010), Jorissen et al (2011, 2013, Decin et al (2011Decin et al ( , 2012, van Hoof et al (2013), and Mečina et al (2014 Sacuto et al (2008) and Paladini et al (in prep.). The MIDI observations do not deviate from spherical symmetry.…”

Section: Herschel/pacsmentioning

confidence: 99%

“…Ueta et al (2006), Jorissen et al (2011), andCox et al (2012) showed that fast-moving AGB stars can alter the wind bubble and produce a bow shock in the direction of the space motion at the interface of the wind and the ISM. For stars with a low space velocity, the CSE appears elliptical (Weaver et al 1977).…”

Section: Origin Of the Elliptical Emissionmentioning

confidence: 99%

Large-scale environments of binary AGB stars probed byHerschel

Mayer

Jorissen

Paladini

et al. 2014

A&A

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Context. The Mass loss of Evolved StarS (MESS) sample observed with PACS on board the Herschel Space Observatory revealed that several asymptotic giant branch (AGB) stars are surrounded by an asymmetric circumstellar envelope (CSE) whose morphology is most likely caused by the interaction with a stellar companion. The evolution of AGB stars in binary systems plays a crucial role in understanding the formation of asymmetries in planetary nebulae (PNe), but at present, only a handful of cases are known where the interaction of a companion with the stellar AGB wind is observed. Aims. We probe the environment of the very evolved AGB star π 1 Gruis on large and small scales to identify the triggers of the observed asymmetries. Methods. Observations made with Herschel/PACS at 70 μm and 160 μm picture the large-scale environment of π 1 Gru. The close surroundings of the star are probed by interferometric observations from the VLTI/AMBER archive. An analysis of the proper motion data of Hipparcos and Tycho-2 together with the Hipparcos Intermediate Astrometric Data help identify the possible cause for the observed asymmetry. Results. The Herschel/PACS images of π 1 Gru show an elliptical CSE whose properties agree with those derived from a CO map published in the literature. In addition, an arc east of the star is visible at a distance of 38 from the primary. This arc is most likely part of an Archimedean spiral caused by an already known G0V companion that is orbiting the primary at a projected distance of 460 au with a period of more than 6200 yr. However, the presence of the elliptical CSE, proper motion variations, and geometric modelling of the VLTI/AMBER observations point towards a third component in the system, with an orbital period shorter than 10 yr, orbiting much closer to the primary than the G0V star.

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“…The resulting fluxes are F ν,12 = 0.207 Jy and F ν,22 = 1.650 Jy at 12 μm and 22 μm, respectively. Adopting the corresponding absorption coefficients of astronomical silicates Q abs,12 = 5.60 × 10 −2 and Q abs,22 = 3.39 × 10 −2 (Draine 1985), the 12 μm and 22 μm fluxes correspond to a temperature of 124 K (for details see Jorissen et al 2011).…”

Section: Dramentioning

confidence: 99%

Search for systemic mass loss in Algols with bow shocks

Mayer

Deschamps

Jorissen

2016

A&A

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Aims. Various studies indicate that interacting binary stars of Algol type evolve non-conservatively. However, direct detections of systemic mass loss in Algols have been scarce so far. We study the systemic mass loss in Algols by looking for the presence of infrared excesses originating from the thermal emission of dust grains, which is linked to the presence of a stellar wind. Methods. In contrast to previous studies, we make use of the fact that stellar and interstellar material is piled up at the edge of the astrosphere where the stellar wind interacts with the interstellar medium. We analyse WISE W3 12 μm and WISE W4 22 μm data of Algol-type binary Be and B[e] stars and the properties of their bow shocks. From the stand-off distance of the bow shock we are able to determine the mass-loss rate of the binary system. Results. Although the velocities of the stars with respect to the interstellar medium are quite low, we find bow shocks present in two systems, namely π Aqr, and ϕ Per; a third system, CX Dra, shows a more irregular circumstellar environment morphology which might somehow be related to systemic mass loss. The properties of the two bow shocks point to mass-loss rates and wind velocities typical of single B stars, which do not support an enhanced systemic mass loss.

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X Herculis and TX Piscium: two cases of ISM interaction with stellar winds observed byHerschel

Cited by 27 publications

References 79 publications

Catching the fish – Constraining stellar parameters for TX Piscium using spectro-interferometric observations

Catching the fish – Constraining stellar parameters for TX Piscium using spectro-interferometric observations

Large-scale environments of binary AGB stars probed byHerschel

Search for systemic mass loss in Algols with bow shocks

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