Lopez, R. Garcia, Natta, A., Caratti O Garatti, A., Ray, T. P., Fedriani, R., Koutoulaki, M., Klarmann, L., Perraut, K., Sanchez-Bermudez, J., Benisty, M., Dougados, C., Labadie, L., Brandner, W., Garcia, P. J. V., Henning, Th., Caselli, P., Duvert, G., de Zeeuw, T., Grellmann, R., Abuter, R., Amorim, A., Bauboeck, M., Berger, J. P., Bonnet, H., Buron, A., Clenet, Y., Coude du Foresto, V., de Wit, W., Eckart, A., Eisenhauer, F., Filho, M., Gao, F., Garcia Dabo, C. E., Gendron, E., Genzel, R., Gillessen, S., Habibi, M., Haubois, X., Haussmann, F., Hippler, S., Hubert, Z., Horrobin, M., Jimenez Rosales, A., Jocou, L., Kervella, P., Kolb, J., Lacour, S., Le Bouquin, J. -B., Lena, P., Ott, T., Paumard, T., Perrin, G., Pfuhl, O., Ramirez, A., Rau, C., Rousset, G., Scheithauer, S., Shangguan, J., Stadler, J., Straub, O., Straubmeier, C., Sturm, E., van Dishoeck, E., Vincent, F., von Fellenberg, S., Widmann, F., Wieprecht, E., Wiest, M., Wiezorrek, E., Woillez, J., Yazici, S. and Zins, G. (2020). A measure of the size of the magnetospheric accretion region in TW Hydrae. Nature, 584 (7822). S. 547 - 556. BERLIN: NATURE RESEARCH. ISSN 1476-4687

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Abstract

Stars form by accreting material from their surrounding disks. There is a consensus that matter flowing through the disk is channelled onto the stellar surface by the stellar magnetic field. This is thought to be strong enough to truncate the disk close to the corotation radius, at which the disk rotates at the same rate as the star. Spectro-interferometric studies in young stellar objects show that hydrogen emission (a well known tracer of accretion activity) mostly comes from a region a few milliarcseconds across, usually located within the dust sublimation radius(1-3). The origin of the hydrogen emission could be the stellar magnetosphere, a rotating wind or a disk. In the case of intermediate-mass Herbig AeBe stars, the fact that Brackett gamma (Br gamma) emission is spatially resolved rules out the possibility that most of the emission comes from the magnetosphere(4-6)because the weak magnetic fields (some tenths of a gauss) detected in these sources(7,8)result in very compact magnetospheres. In the case of T Tauri sources, their larger magnetospheres should make them easier to resolve. The small angular size of the magnetosphere (a few tenths of a milliarcsecond), however, along with the presence of winds(9,10)make the interpretation of the observations challenging. Here we report optical long-baseline interferometric observations that spatially resolve the inner disk of the T Tauri star TW Hydrae. We find that the near-infrared hydrogen emission comes from a region approximately 3.5 stellar radii across. This region is within the continuum dusty disk emitting region (7 stellar radii across) and also within the corotation radius, which is twice as big. This indicates that the hydrogen emission originates in the accretion columns (funnel flows of matter accreting onto the star), as expected in magnetospheric accretion models, rather than in a wind emitted at much larger distance (more than one astronomical unit). The size of the inner disk of the T Tauri star TW Hydrae is determined using optical long-baseline interferometric observations, indicating that hydrogen emission comes from a region approximately 3.5 stellar radii across.

Item Type: Journal Article
Creators:
CreatorsEmailORCIDORCID Put Code
Lopez, R. GarciaUNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Natta, A.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Caratti O Garatti, A.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Ray, T. P.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Fedriani, R.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Koutoulaki, M.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Klarmann, L.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Perraut, K.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Sanchez-Bermudez, J.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Benisty, M.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Dougados, C.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Labadie, L.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Brandner, W.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Garcia, P. J. V.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Henning, Th.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Caselli, P.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Duvert, G.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
de Zeeuw, T.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Grellmann, R.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Abuter, R.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Amorim, A.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Bauboeck, M.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Berger, J. P.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Bonnet, H.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Buron, A.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Clenet, Y.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Coude du Foresto, V.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
de Wit, W.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Eckart, A.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Eisenhauer, F.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Filho, M.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Gao, F.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Garcia Dabo, C. E.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Gendron, E.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Genzel, R.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Gillessen, S.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Habibi, M.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Haubois, X.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Haussmann, F.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Hippler, S.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Hubert, Z.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Horrobin, M.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Jimenez Rosales, A.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Jocou, L.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Kervella, P.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Kolb, J.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Lacour, S.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Le Bouquin, J. -B.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Lena, P.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Ott, T.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Paumard, T.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Perrin, G.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Pfuhl, O.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Ramirez, A.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Rau, C.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Rousset, G.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Scheithauer, S.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Shangguan, J.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Stadler, J.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Straub, O.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Straubmeier, C.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Sturm, E.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
van Dishoeck, E.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Vincent, F.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
von Fellenberg, S.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Widmann, F.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Wieprecht, E.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Wiest, M.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Wiezorrek, E.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Woillez, J.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Yazici, S.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Zins, G.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
URN: urn:nbn:de:hbz:38-322538
DOI: 10.1038/s41586-020-2613-1
Journal or Publication Title: Nature
Volume: 584
Number: 7822
Page Range: S. 547 - 556
Date: 2020
Publisher: NATURE RESEARCH
Place of Publication: BERLIN
ISSN: 1476-4687
Language: English
Faculty: Unspecified
Divisions: Unspecified
Subjects: no entry
Uncontrolled Keywords:
KeywordsLanguage
HERBIG AE/BE STARS; MAGNETIC-FIELDS; TAURI STARS; DISK ACCRETION; EMISSION; HYDROGEN; PLANET; TESTSMultiple languages
Multidisciplinary SciencesMultiple languages
URI: http://kups.ub.uni-koeln.de/id/eprint/32253

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