Is protostellar heating sufficient to halt fragmentation? A case study of the massive protocluster G8.68-0.37

TL;DR

This study investigates whether protostellar heating can prevent fragmentation in star-forming regions, concluding that external mass accretion is essential for forming massive stars rather than isolated core collapse.

Contribution

The paper combines observations and modeling to challenge the idea that protostellar heating alone halts fragmentation, emphasizing the importance of external mass inflow for massive star formation.

Findings

Protostellar heating alone cannot prevent fragmentation in massive star-forming regions.

Massive stars likely form through accretion from larger-scale gas reservoirs.

Observed cores require additional mass inflow to reach the mass of O stars.

Abstract

If star formation proceeds by thermal fragmentation and the subsequent gravitational collapse of the individual fragments, how is it possible to form fragments massive enough for O and B stars in a typical star-forming molecular cloud where the Jeans mass is about 1Msun at the typical densities (10^4 cm^-3) and temperatures (10K)? We test the hypothesis that a first generation of low-mass stars may heat the gas enough that subsequent thermal fragmentation results in fragments >=10Msun, sufficient to form B stars. We combine ATCA and SMA observations of the massive star-forming region G8.68-0.37 with radiative transfer modeling to derive the present-day conditions in the region and use this to infer the conditions in the past, at the time of core formation. Assuming the current mass/separation of the observed cores equals the fragmentation Jeans mass/length and the region's average density has not changed, requires the gas temperature to have been 100K at the time of fragmentation. The postulated first-generation of low-mass stars would still be around today, but the number required to heat the cloud exceeds the limits imposed by the observations. Several lines of evidence suggest the observed cores in the region should eventually form O stars yet none have sufficient raw material. Even if feedback may have suppressed fragmentation, it was not sufficient to halt it to this extent. To develop into O stars, the cores must obtain additional mass from outside their observationally defined boundaries. The observations suggest they are currently fed via infall from the very massive reservoir (~1500Msun) of gas in the larger pc scale cloud around the star-forming cores. This suggests that massive stars do not form in the collapse of individual massive fragments, but rather in smaller fragments that themselves continue to gain mass by accretion from larger scales.