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| Fältnamn | Indikatorer | Metadata |
|---|---|---|
| 000 | 05551naa a2200973 4500 | |
| 001 | oai:DiVA.org:su-161190 | |
| 003 | SwePub | |
| 008 | 181102s2018 | |||||||||||000 ||eng| | |
| 024 | 7 | a https://urn.kb.se/resolve?urn=urn:nbn:se:su:diva-1611902 URI |
| 024 | 7 | a https://doi.org/10.1051/0004-6361/2018325832 DOI |
| 040 | a (SwePub)su | |
| 041 | a engb eng | |
| 042 | 9 SwePub | |
| 072 | 7 | a ref2 swepub-contenttype |
| 072 | 7 | a art2 swepub-publicationtype |
| 100 | 1 | a Olofsson, J.4 aut |
| 245 | 1 0 | a Resolving faint structures in the debris disk around TWA 7 Tentative detections of an outer belt, a spiral arm, and a dusty cloud |
| 264 | c 2018-09-26 | |
| 264 | 1 | b EDP Sciences,c 2018 |
| 338 | a print2 rdacarrier | |
| 520 | a Context. Debris disks are the intrinsic by-products of the star and planet formation processes. Most likely due to instrumental limitations and their natural faintness, little is known about debris disks around low mass stars, especially when it comes to spatially resolved observations. Aims. We present new VLT/SPHERE IRDIS dual-polarization imaging (DPI) observations in which we detect the dust ring around the M2 spectral type star TWA 7. Combined with additional angular differential imaging observations we aim at a fine characterization of the debris disk and setting constraints on the presence of low-mass planets. Methods. We modeled the SPHERE DPI observations and constrain the location of the small dust grains, as well as the spectral energy distribution of the debris disk, using the results inferred from the observations, and performed simple N-body simulations. Results. We find that the dust density distribution peaks at similar to 0.72 '' (25 au), with a very shallow outer power-law slope, and that the disk has an inclination of similar to 13 degrees with a position angle of similar to 91 degrees east of north. We also report low signal-to-noise ratio detections of an outer belt at a distance of similar to 1.5 '' (similar to 52 au) from the star, of a spiral arm in the southern side of the star, and of a possible dusty clump at 0.11 ''. These findings seem to persist over timescales of at least a year. Using the intensity images, we do not detect any planets in the close vicinity of the star, but the sensitivity reaches Jovian planet mass upper limits. We find that the SED is best reproduced with an inner disk at similar to 0.2 '' (similar to 7 au) and another belt at 0.72 '' (25 au). Conclusions. We report the detections of several unexpected features in the disk around TWA 7. A yet undetected 100 M-circle plus planet with a semi-major axis at 20-30 au could possibly explain the outer belt as well as the spiral arm. We conclude that stellar winds are unlikely to be responsible for the spiral arm. | |
| 650 | 7 | a NATURVETENSKAPx Fysikx Astronomi, astrofysik och kosmologi0 (SwePub)103052 hsv//swe |
| 650 | 7 | a NATURAL SCIENCESx Physical Sciencesx Astronomy, Astrophysics and Cosmology0 (SwePub)103052 hsv//eng |
| 653 | a circumstellar matter | |
| 653 | a instrumentation: high angular resolution | |
| 653 | a instrumentation: polarimeters | |
| 700 | 1 | a van Holstein, R. G.4 aut |
| 700 | 1 | a Boccaletti, A.4 aut |
| 700 | 1 | a Janson, Markusu Stockholms universitet,Institutionen för astronomi,Max Planck Institut für Astronomie, Germany4 aut0 (Swepub:su)mjanso |
| 700 | 1 | a Thebault, P.4 aut |
| 700 | 1 | a Gratton, R.4 aut |
| 700 | 1 | a Lazzoni, C.4 aut |
| 700 | 1 | a Kral, Q.4 aut |
| 700 | 1 | a Bayo, A.4 aut |
| 700 | 1 | a Canovas, H.4 aut |
| 700 | 1 | a Caceres, C.4 aut |
| 700 | 1 | a Ginski, C.4 aut |
| 700 | 1 | a Pinte, C.4 aut |
| 700 | 1 | a Asensio-Torres, Rubenu Stockholms universitet,Institutionen för astronomi4 aut0 (Swepub:su)rasen |
| 700 | 1 | a Chauvin, G.4 aut |
| 700 | 1 | a Desidera, S.4 aut |
| 700 | 1 | a Henning, Th4 aut |
| 700 | 1 | a Langlois, M.4 aut |
| 700 | 1 | a Milli, J.4 aut |
| 700 | 1 | a Schlieder, J. E.4 aut |
| 700 | 1 | a Schreiber, M. R.4 aut |
| 700 | 1 | a Augereau, J-C4 aut |
| 700 | 1 | a Bonnefoy, M.4 aut |
| 700 | 1 | a Buenzli, E.4 aut |
| 700 | 1 | a Brandner, W.4 aut |
| 700 | 1 | a Durkan, Stephenu Stockholms universitet,Institutionen för astronomi,Queen’s University Belfast, Northern Ireland, UK4 aut |
| 700 | 1 | a Engler, N.4 aut |
| 700 | 1 | a Feldt, M.4 aut |
| 700 | 1 | a Godoy, N.4 aut |
| 700 | 1 | a Grady, C.4 aut |
| 700 | 1 | a Hagelberg, J.4 aut |
| 700 | 1 | a Lagrange, A-M4 aut |
| 700 | 1 | a Lannier, J.4 aut |
| 700 | 1 | a Ligi, R.4 aut |
| 700 | 1 | a Maire, A-L4 aut |
| 700 | 1 | a Mawet, D.4 aut |
| 700 | 1 | a Menard, F.4 aut |
| 700 | 1 | a Mesa, D.4 aut |
| 700 | 1 | a Mouillet, D.4 aut |
| 700 | 1 | a Peretti, S.4 aut |
| 700 | 1 | a Perrot, C.4 aut |
| 700 | 1 | a Salter, G.4 aut |
| 700 | 1 | a Schmidt, T.4 aut |
| 700 | 1 | a Sissa, E.4 aut |
| 700 | 1 | a Thalmann, C.4 aut |
| 700 | 1 | a Vigan, A.4 aut |
| 700 | 1 | a Abe, L.4 aut |
| 700 | 1 | a Feautrier, P.4 aut |
| 700 | 1 | a Le Mignant, D.4 aut |
| 700 | 1 | a Moulin, T.4 aut |
| 700 | 1 | a Pavlov, A.4 aut |
| 700 | 1 | a Rabou, P.4 aut |
| 700 | 1 | a Rousset, G.4 aut |
| 700 | 1 | a Roux, A.4 aut |
| 710 | 2 | a Stockholms universitetb Institutionen för astronomi4 org |
| 773 | 0 | t Astronomy and Astrophysicsd : EDP Sciencesg 617q 617x 0004-6361x 1432-0746 |
| 856 | 4 | u https://www.aanda.org/articles/aa/pdf/2018/09/aa32583-18.pdf |
| 856 | 4 8 | u https://urn.kb.se/resolve?urn=urn:nbn:se:su:diva-161190 |
| 856 | 4 8 | u https://doi.org/10.1051/0004-6361/201832583 |
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- Lazzoni, C.
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- Chauvin, G.
- Desidera, S.
- Henning, Th
- Langlois, M.
- Milli, J.
- Schlieder, J. E.
- Schreiber, M. R.
- Augereau, J-C
- Bonnefoy, M.
- Buenzli, E.
- Brandner, W.
- Durkan, Stephen
- Engler, N.
- Feldt, M.
- Godoy, N.
- Grady, C.
- Hagelberg, J.
- Lagrange, A-M
- Lannier, J.
- Ligi, R.
- Maire, A-L
- Mawet, D.
- Menard, F.
- Mesa, D.
- Mouillet, D.
- Peretti, S.
- Perrot, C.
- Salter, G.
- Schmidt, T.
- Sissa, E.
- Thalmann, C.
- Vigan, A.
- Abe, L.
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