resolving dust and gas structures in protoplanetary disks

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While the emergent line intensity depends on the underlying molecular abundance, other factors including the disk density and temperature structure affect the emerging lines

Both sources with large amounts of dust settling (DQ Tau) and small amounts (V806 Tau) can present similarly bright and resolved CO emission lines ( ∼40 mJy bm −1 ); the results

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Alternatively, if the reconnection events provide a necessary pathway for accretion processes, then the haphazard nature of magnetic fields easily could explain the variability in

The recorded activity is consistent with the proposed picture for synchrotron emission initiated by a magnetic reconnection event when the two stellar magnetospheres of the

Since in both the DQ Tau and UZ Tau E cases, optical brightenings are common near periastron due to periodic accretion events (Jensen et al. 2007), and because the optical light

Our instrument design to probe the collisions of fragile particles at low velocities proved successful in its inaugural run at ambient temperatures (300 K) in vacuum, as well as