The JCMT Gould Belt Survey: radiative heating by OB stars. (arXiv:2105.03353v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Rumble_D/0/1/0/all/0/1">Damian Rumble</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hatchell_J/0/1/0/all/0/1">Jennifer Hatchell</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kirk_H/0/1/0/all/0/1">Helen Kirk</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pattle_K/0/1/0/all/0/1">Kate Pattle</a>
Radiative feedback can influence subsequent star formation. We quantify the
heating from OB stars in the local star-forming regions in the JCMT Gould Belt
survey. Dust temperatures are calculated from 450/850 micron flux ratios from
SCUBA-2 observations at the JCMT assuming a fixed dust opacity spectral index
$beta=1.8$. Mean dust temperatures are calculated for each submillimetre clump
along with projected distances from the main OB star in the region. Temperature
vs. distance is fit with a simple model of dust heating by the OB star
radiation plus the interstellar radiation field and dust cooling through
optically thin radiation. Classifying the heating sources by spectral type,
O-type stars produce the greatest clump average temperature rises and largest
heating extent, with temperatures over 40 K and significant heating out to at
least 2.4 pc. Early-type B stars (B4 and above) produce temperatures of over 20
K and significant heating over 0.4 pc. Late-type B stars show a marginal
heating effect within 0.2 pc. For a given projected distance, there is a
significant scatter in clump temperatures that is due to local heating by other
luminous stars in the region, projection effects, or shadowing effects. Even in
these local, `low-mass’ star-forming regions, radiative feedback is having an
effect on parsec scales, with 24% of the clumps heated to at least 3 K above
the 15 K base temperature expected from heating by only the interstellar
radiation field, and a mean dust temperature for heated clumps of 24 K.
Radiative feedback can influence subsequent star formation. We quantify the
heating from OB stars in the local star-forming regions in the JCMT Gould Belt
survey. Dust temperatures are calculated from 450/850 micron flux ratios from
SCUBA-2 observations at the JCMT assuming a fixed dust opacity spectral index
$beta=1.8$. Mean dust temperatures are calculated for each submillimetre clump
along with projected distances from the main OB star in the region. Temperature
vs. distance is fit with a simple model of dust heating by the OB star
radiation plus the interstellar radiation field and dust cooling through
optically thin radiation. Classifying the heating sources by spectral type,
O-type stars produce the greatest clump average temperature rises and largest
heating extent, with temperatures over 40 K and significant heating out to at
least 2.4 pc. Early-type B stars (B4 and above) produce temperatures of over 20
K and significant heating over 0.4 pc. Late-type B stars show a marginal
heating effect within 0.2 pc. For a given projected distance, there is a
significant scatter in clump temperatures that is due to local heating by other
luminous stars in the region, projection effects, or shadowing effects. Even in
these local, `low-mass’ star-forming regions, radiative feedback is having an
effect on parsec scales, with 24% of the clumps heated to at least 3 K above
the 15 K base temperature expected from heating by only the interstellar
radiation field, and a mean dust temperature for heated clumps of 24 K.
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