Variable Warm Dust around the Herbig Ae Star HD 169142: Birth of a Ring?*

Chen, L.; Moór, A.; Kreplin, Alexander; Kóspál, Á.; Ábrahám, P.; Matter, A.; Hofmann, K.-H.; Schertl, D.; Weigelt, G.

doi:10.3847/2041-8213/ab59dd

Cited by 10 publications

(6 citation statements)

References 39 publications

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“…It is difficult to constrain such scenarios with our observations, as simultaneous photometric and interferometric campaigns should be carefully planned to address this issue. However, we note that structural variability was already inferred in some objects, in particular in transition disks, from photometric, spectroscopic and interferometric studies (Espaillat et al 2011(Espaillat et al , 2014Chen et al 2019).…”

Section: Discussionmentioning

confidence: 58%

Probing inner and outer disk misalignments in transition disks

Bohn

Benisty

Perraut

et al. 2022

A&A

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Context. Transition disks are protoplanetary disks with dust-depleted cavities, possibly indicating substantial clearing of their dust content by a massive companion. For several known transition disks, dark regions interpreted as shadows have been observed in scattered light imaging and are hypothesized to originate from misalignments between distinct regions of the disk. Aims. We aim to investigate the presence of misalignments in transition disks. We study the inner disk (<1 au) geometries of a sample of 20 well-known transition disks with Very Large Telescope Interferometer (VLTI) GRAVITY observations and use complementary 12CO and 13CO molecular line archival data from the Atacama Large Millimeter/submillimeter Array (ALMA) to derive the orientation of the outer disk regions (>10 au). Methods. We fit simple parametric models to the visibilities and closure phases of the GRAVITY data to derive the inclination and position angle of the inner disks. The outer disk geometries were derived from Keplerian fits to the ALMA velocity maps and compared to the inner disk constraints. We also predicted the locations of expected shadows for significantly misaligned systems. Results. Our analysis reveals six disks to exhibit significant misalignments between their inner and outer disk structures. The predicted shadow positions agree well with the scattered light images of HD 100453 and HD 142527, and we find supporting evidence for a shadow in the south of the disk around CQ Tau. In the other three targets for which we infer significantly misaligned disks, V1247 Ori, V1366 Ori, and RY Lup, we do not see any evident sign of shadows in the scattered light images. The scattered light shadows observed in DoAr 44, HD 135344 B, and HD 139614 are consistent with our observations, yet the underlying morphology is likely too complex to be described properly by our models and the accuracy achieved by our observations. Conclusions. The combination of near infrared and submillimeter interferometric observations allows us to assess the geometries of the innermost disk regions and those of the outer disk. Whereas we can derive precise constraints on the potential shadow positions for well-resolved inner disks around Herbig Ae/Be stars, the large statistical uncertainties for the marginally resolved inner disks around the T Tauri stars of our sample make it difficult to extract conclusive constraints for the presence of shadows in these systems.

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Section: Discussionmentioning

confidence: 58%

Probing inner and outer disk misalignments in transition disks

Bohn

Benisty

Perraut

et al. 2022

A&A

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“…Yet, HD 169142 is a Herbig F1 star (Gray et al 2017) with a mass of 1.7 M (Blondel & Djie 2006) at 114.9 ± 0.4 pc (Gaia Collaboration et al 2018 with its surrounding disk seen almost face-on (i = 13 ± 1 • , Raman et al 2006;Panić et al 2008). A small (∼ 0.3 AU) and variable NIR inner dust disk has been observed in HD 169142 (Wagner et al 2015;Chen et al 2019). This inner dust disk has also been detected in high resolution ALMA observations (Pérez et al 2019).…”

Section: The Sourcesmentioning

confidence: 97%

Gas temperature structure across transition disk cavities

Leemker,

Booth,

van Dishoeck

et al. 2022

Preprint

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Context.Most disks observed at high angular resolution show signs of substructures like rings, gaps, arcs, and cavities in both the gas and the dust. To understand the physical mechanisms responsible for these structures, knowledge about the gas surface density is essential. This, in turn, requires information on the gas temperature. Aims. The aim of this work is to constrain the gas temperature as well as the gas surface densities inside and outside the mm-dust cavities of two transition disks: LkCa15 and HD 169142, with dust cavities of 68 AU and 25 AU, respectively. Methods. We use some of the few existing ALMA observations of the J = 6 − 5 transition of 13 CO together with archival J = 2 − 1 data of 12 CO, 13 CO and C 18 O. The ratio of the 13 CO J = 6 − 5 to the J = 2 − 1 transition is used to constrain the temperature and is compared with that found from peak brightness temperature of optically thick lines. The spectra are used to resolve the innermost disk regions to a spatial resolution better than the beam of the observations. Furthermore, we use the thermochemical code DALI to model the temperature and density structure of a typical transition disk as well as the emitting regions of the CO isotopologues. Results. The 13 CO J = 6−5 and J = 2−1 transitions peak inside the dust cavity in both disks, indicating that gas is present in the dust cavities. The kinematically derived radial profiles show that the gas is detected down to 10 and 5 − 10 AU, much further in than the dust cavities in the LkCa15 and HD 169142 disks, respectively. For LkCa15, the steep increase towards the star in the 13 CO J = 6 − 5 transition, in contrast to the J = 2 − 1 line, shows that the gas is too warm to be traced by the J = 2 − 1 line and that molecular excitation is important for analysing the line emission. Quantitatively, the 6 − 5/2 − 1 line ratio constrains the gas temperature in the emitting layers inside the dust cavity to be up to 65 K, warmer than in the outer disk at 20−30 K. For the HD 169142, the lines are optically thick, complicating a line ratio analysis. In this case, the peak brightness temperature constrains the gas in the dust cavity of HD 169142 to be 170 K, whereas that in the outer disk is only 100 K. The data indicate a vertical structure in which the 13 CO 6 − 5 line emits from a higher layer than the 2 − 1 line in both disks, consistent with exploratory thermo-chemical DALI models. Such models also show that a more luminous central star, a lower abundance of PAHs and the absence of a dusty inner disk increase the temperature of the emitting layers and hence the line ratio in the gas cavity. The gas column density in the LkCa15 dust cavity drops by a factor > 2 compared to the outer disk, with an additional drop of an order of magnitude inside the gas cavity at 10 AU. In the case of HD 169142, the gas column density drops by a factor of 200−500 inside the gas cavity. Conclusions. The gas temperatures inside the dust cavities steeply increase towards the star and reach temperatures up to 65 K (LkCa15) an...

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“…2018 márciusában magyar csillagászok is részt vettek Chilében a MATISSE üzembe helyezésében. jelű közepes tömegű fiatal csillagról készítettek több alkalommal 1,65 mikrométeren interferometrikus méréseket (Chen et al, 2019). Az adatok vizsgálatából kiderült, hogy a csillag körül valószínűleg korábban létrejött planetezimálok, bolygókezdemények összeütközése nyomán egy törmelékből álló gyűrű jött létre a csillagtól kb.…”

Section: Magyar Hozzájárulás Interferometriai Kutatásokhoz éS Műszerfunclassified

Az optikai interferometria 100 éve a csillagászatban • 100 Years of Optical Interferometry in Astronomy

Kóspál¹

2020

Ma.Tud.

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Idén ünnepeljük a 100. évfordulóját annak, hogy először sikerült megmérni egy olyan csillag látszó átmérőjét, amely nem a mi Napunk. A méréshez az interferometria módszerét használták, amelynek csillagászati alkalmazása a 19. század végére nyúlik vissza, de a mai napig töretlenül népszerű, és számos alapvető fontosságú csillagászati felfedezést értek el ezzel a technikával. Ebben a cikkben bemutatom Michelson és kollégái híres kísérletét, amellyel meghatározták a Betelgeuze nevű vörös szuperóriás csillag látszó átmérőjét. Azt is áttekintem, hogyan fejlődött azóta a csillagászati interferometria, és mit tanultunk erről a csillagról az új műszereknek köszönhetően. Végül röviden összefoglalom az interferometriai kutatásokhoz és műszerfejlesztésekhez való magyar hozzájárulást.

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Variable Warm Dust around the Herbig Ae Star HD 169142: Birth of a Ring?*

Cited by 10 publications

References 39 publications

Probing inner and outer disk misalignments in transition disks

Probing inner and outer disk misalignments in transition disks

Gas temperature structure across transition disk cavities

Az optikai interferometria 100 éve a csillagászatban • 100 Years of Optical Interferometry in Astronomy

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