Fragmenting protostellar disks: properties and observational signatures

TL;DR

This study uses hydrodynamic simulations to analyze gravitational fragmentation in protostellar disks, assessing the properties of fragments and their potential detection with ALMA at various distances and resolutions.

Contribution

It provides new insights into the mass, distribution, and observational signatures of fragments formed during protostellar disk fragmentation.

Findings

Fragments range from Jupiter mass to very-low-mass protostars

ALMA can detect fragments as small as 1.5 M_Jup at 800 AU with 1-hour integration

Detection likelihood decreases with lower resolution

Abstract

Using numerical hydrodynamic simulations, we study the gravitational fragmentation of an unstable protostellar disc formed during the collapse of a pre-stellar core with a mass of 1.2 M_sun. The forming fragments span a mass range from about a Jupiter mass to very-low-mass protostars and are located at distances from a few tens to a thousand AU, with a dearth of objects at < 100 AU. We explore the possibility of observational detection of the fragments in discs viewed through the outflow cavity at a distance of 250 pc. We demonstrate that one hour of integration time with the Atacama Large Millimeter/sub-millimeter Array (ALMA) is sufficient to detect the fragments with masses as low as 1.5 M_Jup at orbital distances up to 800 AU from the protostar. The ALMA resolution sets the limit on the minimum orbital distance of detectable fragments. For the adopted resolution of our simulated ALMA images of 0.1", the fragments can be detected at distances down to 50 AU. At smaller distances, the fragments usually merge with the central density peak. The likelihood for detecting the fragments reduces significantly for a lower resolution of 0.5". Some of the most massive fragments, regardless of their orbital distance, can produce characteristic peaks at approximately 5 micron and hence their presence can be indirectly inferred from the observed spectral energy distributions of protostars.