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23 April 2024 |
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Imaging the photoevaporating disk and radio jet of GM Aur | | Enrique Macias
; Guillem Anglada
; Mayra Osorio
; Nuria Calvet
; Jose M. Torrelles
; Jose F. Gomez
; Catherine Espaillat
; Susana Lizano
; Luis F. Rodriguez
; Carlos Carrasco-Gonzalez
; Luis Zapata
; | | Date: |
14 Jul 2016 | | Abstract: | Photoevaporation is probably the main agent for gas dispersal during the last
stages of protoplanetary disk evolution. However, the overall mass loss rate in
the photoevaporative wind and its driving mechanism are still not well
understood. Here we report multi-configuration Very Large Array observations at
0.7, 3, and 5 cm towards the transitional disk of GM Aur. Our radio continuum
observations allow us to image and spatially resolve, for the first time, the
three main components at work in this stage of the disk evolution: the disk of
dust, the ionized radio jet perpendicular to it, and the photoevaporative wind
arising from the disk. The mass loss rate inferred from the flux density of the
radio jet is consistent with the ratio between ejection and accretion rates
found in younger objects, suggesting that transitional disks can power
collimated ejections of material apparently following the same physical
mechanisms as much younger protostars. Our results indicate that extreme-UV
(EUV) radiation is the main ionizing mechanism of the photoevaporative wind
traced by the free-free emission. The required low EUV photon luminosity of
$sim6 imes10^{40}$ s$^{-1}$ would produce a photoevaporation rate of only
$dot{M}_{
m w,EUV}simeq1.3 imes10^{-10}~M_{odot}$ yr$^{-1}$. Therefore,
other mechanisms are required to disperse the disk in the timescale imposed by
observations. | | Source: | arXiv, 1607.4225 | | Services: | Forum | Review | PDF | Favorites | |
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