From the atmosphere to the circumstellar environment in cool evolved stars

Wittkowski, M.; Paladini, C.

doi:10.1051/eas/1569009

Cited by 3 publications

(5 citation statements)

References 111 publications

(125 reference statements)

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“…The details of dust formation and acceleration process are matter of discussion [Sect. 3,3]. Departure from spherical symmetry have been observed also in the dust forming region (∼ 10 µm), at the onset of stellar wind.…”

Section: The Dust-forming Regionmentioning

confidence: 97%

“…While 3D models are still under development [22,23,10], observational astronomers, and more precisely optical interferometrists, should push to obtain more images, and also to compare the observations with 1D available models. A summary of what has been done with 1D models is available in [3], nevertheless I would like to mention here a few interesting developments occurred in the field of RSG over the last few years. Usually 1D models successfully reproduce spectroscopy and photometric data.…”

Section: Photosphere and Inner Molecular Environmentmentioning

confidence: 99%

“…With 2-dimensional information, I mean the possible asymmetric For further information e-mail to paladini@ulb.ac.be structures that have been detected so far (via visibility model-fitting, direct closure phase and differential phase measurements), and their interpretation. Interested readers may want to consult also earlier reviews on the topic [1,2,3]. Results obtained with other interferometric techniques such as aperture masking or speckle interferometry are not covered here.…”

Section: Introductionmentioning

confidence: 99%

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Evolved stars at high angular resolution: present and future

Paladini

2016

SPIE Proceedings

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The late evolutionary stages of stellar evolution are a key ingredient for our understanding in many fields of astrophysics, including stellar evolution and the enrichment of the interstellar medium (ISM) via stellar yields. Already the first interferometric campaigns identified evolved stars as the primary targets because of their extended and partially optically thin atmospheres, and the brightness in the infrared. Interferometric studies spanning different wavelength ranges, from visual to mid-infrared, have greatly increased our knowledge of the complex atmospheres of these objects where different dynamic processes are at play. In less than two decades this technique went from measuring simple diameters to produce the first images of stellar surfaces. By scanning the extended atmospheres we constrained theoretical models, learnt about molecular stratification, dust formation, and stellar winds, and there is still a lot to be done. In this contribution I will review the recent results that optical/infrared interferometry has made on our current understanding of cool evolved stars. The presentation will focus on asymptotic giant branch stars, and red supergiants. I will discuss the challenges of image reconstruction, and highlight how this field of research will benefit from the synergy of the current interferometric instrument(s) with the second generation VLTI facilities GRAVITY and MATISSE. Finally I will conclude with a short introspection on applications of a visible interferometer and of the the Planet Formation Imager (PFI) to the field of evolved stars.

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Section: The Dust-forming Regionmentioning

confidence: 97%

Section: Photosphere and Inner Molecular Environmentmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Evolved stars at high angular resolution: present and future

Paladini

2016

SPIE Proceedings

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“…The recent studies of the stratification of the dynamic atmosphere of evolved stars (see ref. 39 or Paladini in this proceeding) are so far limited to nearby objects with solar metallicity. Such kind of works, especially when it comes to comparison with model atmospheres, are hampered by distance uncertainties.…”

Section: Secondary Science Cases: Stellar Astrophysicsmentioning

confidence: 99%

Planet Formation Imager (PFI): science vision and key requirements

Kraus

Ireland

et al. 2016

SPIE Proceedings

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The Planet Formation Imager (PFI) project aims to provide a strong scientific vision for ground-based optical astronomy beyond the upcoming generation of Extremely Large Telescopes. We make the case that a breakthrough in angular resolution imaging capabilities is required in order to unravel the processes involved in planet formation. PFI will be optimised to provide a complete census of the protoplanet population at all stellocentric radii and over the age range from 0.1 to ∼ 100 Myr. Within this age period, planetary systems undergo dramatic changes and the final architecture of planetary systems is determined. Our goal is to study the planetary birth on the natural spatial scale where the material is assembled, which is the "Hill Sphere" of the forming planet, and to characterise the protoplanetary cores by measuring their masses and physical properties. Our science working group has investigated the observational characteristics of these young protoplanets as well as the migration mechanisms that might alter the system architecture. We simulated the imprints that the planets leave in the disk and study how PFI could revolutionise areas ranging from exoplanet to extragalactic science. In this contribution we outline the key science drivers of PFI and discuss the requirements that will guide the technology choices, the site selection, and potential science/technology tradeoffs.Our preliminary results indicate that the shorter-wavelength L and M bands are optimal for detecting the circumplanetary disk in spectral line tracers. Line observations offer the prospect to detect even very low-mass

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“…Actual data from the narrow spectral regions shown along the bottom left side of the plot indicate the very limited amount of bandwidth (distributed within 217-221 GHz) that could be employed using the current ALMA system for the high angular and spectral resolution (∼ 0.1 km s −1 ) follow-up of G358.93-0.03. and evolved stars in our Milky Way to the nuclear disks of luminous galaxies (see for example Hirota et al 2014;Wittkowski & Paladini 2014;Kameno et al 2023). Band 7 covers two particularly diagnostic water maser transitions at 321 and 325 GHz with E lower of 1846 K and 453 K, respectively (Neufeld & Melnick 1990;Menten et al 1990).…”

Section: Band 7v2 Examplementioning

confidence: 99%

Expanded Maser Science Opportunities with the ALMA Wideband Sensitivity Upgrade

Brogan

2022

Proc. IAU

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The ALMA Project is embarking on a partner-wide initiative to at least double, and ultimately quadruple the correlated bandwidth of ALMA by @2030. This initiative is called the ALMA Wideband Sensitivity Upgrade (WSU). In this contribution, I briefly describe the main aspects of the upgrade and status. Then I provide several examples of how the WSU will enhance (sub)millimeter maser science by affording the ability to observe more diagnostic maser transitions (and thermal lines) with a single observation.

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From the atmosphere to the circumstellar environment in cool evolved stars

Cited by 3 publications

References 111 publications

Evolved stars at high angular resolution: present and future

Evolved stars at high angular resolution: present and future

Planet Formation Imager (PFI): science vision and key requirements

Expanded Maser Science Opportunities with the ALMA Wideband Sensitivity Upgrade

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