About the possibility to detect brown dwarfs in typical debris disks from spectral energy distributions
|1Zakhozhay, OV |
1Main Astronomical Observatory of the National Academy of Sciences of Ukraine, Kyiv, Ukraine
|Kinemat. fiz. nebesnyh tel (Online) 2015, 31(4):39-44|
|Start Page: Physics of Stars and Interstellar Medium|
When planets and brown dwarfs are formed in protoplanetary disks, they clear gaps along their orbits. We investigate the possibility to identify these gaps and hence to detect the presence of planetary or substellar companions in debris disk via spectral energy distributions. We present the results for a modelled system at 100 Myrs, with a low-mass stellar object surrounded by a typical debris disk that includes embedded substellar companion. The width of the gap opened by the companion is determined as the diameter of the Hill sphere of the substellar companion.
|Keywords: cavity, orbital movement|
1.I. Baraffe, G. Chabrier, F. Allard, and P. H. Hauschildt, “Evolutionary models for solar metallicity low-mass stars: Mass-magnitude relationships and color-magnitude diagrams,” Astron. Astrophys. 337, 403–412 (1998).
2.J. Carpenter, J. Bouwman, E. E. Mamajek, et al., “Formation and evolution of planetary systems: Properties of debris dust around solar-type stars,” Astrophys. J., Suppl. Ser. 181, 197–226 (2009).
3.J. K. Donaldson, J. Lebreton, A. Roberge, et al., “Modeling the HD32297 debris disk with far-IR HERSCHEL data,” Astrophys. J. 772, 17–26 (2013).
4.J. K. Donaldson, A. Roberge, C. H. Chen, et al., “HERSCHEL PACS observations and modeling of debris disks in the Tucana-Horologium association,” Astrophys. J. 753, 147–158 (2012).
5.B. T. Draine, “On the submillimeter opacity of protoplanetary disks,” Astrophys. J. 636, 1114–1120 (2006).
6.S. Ertel, S. Wolf, and J. Rodmann, “Observing planet-disk interaction on debris disks,” Astron. Astrophys. 544, A61–A76 (2012).
7.A. Johansen, J. Blum, H. Tanaka, et al., “The multifaceted planetesimal formation process,” in Protostars and Planets VI, Ed. by H. Beuther, R. Klessen, C. Dullemond, and Th. Henning (University of Arizona Press, Tucson, 2014), 547–570.
8.A. M. Hughes, D. J. Wilner, S. M. Andrews, et al., “Resolved submillimeter observation of the Hr 8799 and HD 107146 debris disks,” Astrophys. J. 740, 38–46 (2011).
9.B. Ma and J. Ge, “Statistical properties of brown dwarf companions: Implications for different formation mechanisms,” Mon. Not. R. Astron. Soc. 439, 2781–2789 (2014).
10.B. C. Matthews, G. Kennedy, B. Sibthorpe, et al., “Resolved imaging of the HR 8799 debris disk with HERSCHEL,” Astrophys. J. 780, 97–108 (2014).
11.A. Moor, P. Abraham, A. Kospal, et al., “A resolved debris disk around the candidate planet-hosting star HD 95086,” Astrophys. Lett. 775, L51–L56 (2013).
12.T. J. Rodigas, R. Malhotra, and P. M. Hinz, “Predictions for shepherding planets in scattered light images of debris disks,” Astrophys. J. 780, 65–74 (2014).
13.P. Thebault, “A new code to study structures in collisionally active, perturbed debris discs: Application to binaries,” Astron. Astrophys. 537, A65–A74 (2012).