A fast bipolar H2 outflow from IRAS 16342−3814: an old star reliving its youth

Gledhill, Tim; Forde, K. P.

doi:10.1111/j.1365-2966.2011.20309.x

Cited by 4 publications

(3 citation statements)

References 63 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The high-mass protostar S255IR NIRS 3 also seems to have a similar morphology, with variability in continuum and CO emission traced to light echoes (Carattio et al 2017). This specific scenario, with H 2 emission from extended winds and CO emission produced by the disk, but seen only in scattered light, also has a direct analog with the post-main-sequence, preplanetary nebula IRAS 16342-3814 (Gledhill & Forde 2012).…”

Section: Interpreting the Brightness Changes In The Infraredmentioning

confidence: 89%

Dissecting the Different Components of the Modest Accretion Bursts of the Very Young Protostar HOPS 373

Yoon

Herczeg

Lee

et al. 2022

ApJ

View full text Add to dashboard Cite

Observed changes in protostellar brightness can be complicated to interpret. In our James Clerk Maxwell Telescope (JCMT) Transient Monitoring Survey, we discovered that a young binary protostar, HOPS 373, is undergoing a modest 30% brightness increase at 850 μm, caused by a factor of 1.8–3.3 enhancement in the accretion rate. The initial burst occurred over a few months, with a sharp rise and then a shallower decay. A second rise occurred soon after the decay, and the source is still bright one year later. The mid-IR emission, the small-scale CO outflow mapped with ALMA, and the location of variable maser emission indicate that the variability is associated with the SW component. The near-IR and NEOWISE W1 and W2 emission is located along the blueshifted CO outflow, spatially offset by ∼3 to 4″ from the SW component. The K-band emission imaged by UKIRT shows a compact H2 emission source at the edge of the outflow, with a tail tracing the outflow back to the source. The W1 emission, likely dominated by scattered light, brightens by 0.7 mag, consistent with expectations based on the submillimeter light curve. The signal of continuum variability in K band and W2 is masked by stable H2 emission, as seen in our Gemini/GNIRS spectrum, and perhaps by CO emission. These differences in emission sources complicate IR searches for variability of the youngest protostars.

show abstract

Section: Interpreting the Brightness Changes In The Infraredmentioning

confidence: 89%

Dissecting the Different Components of the Modest Accretion Bursts of the Very Young Protostar HOPS 373

Yoon

Herczeg

Lee

et al. 2022

ApJ

View full text Add to dashboard Cite

show abstract

“…Line map units are in erg s −1 cm −2 . These results can be compared to K-band integral field spectroscopy that reveals bipolar (> 150 km s −1 ) H2 outflows such as associated with IRAS 16342 − 3814 Gledhill & Forde (2012) and Gledhill & Forde (2015).…”

Section: Emission Mapsmentioning

confidence: 99%

Numerical simulations of wind-driven protoplanetary nebulae – I. near-infrared emission

Новиков

Smith

2018

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

To understand how the circumstellar environments of post-AGB stars develop into planetary nebulae, we initiate a systematic study of 2D axisymmetric hydrodynamic simulations of protoplanetary nebula (pPN) with a modified ZEUS code. The aim of this first work is to compare the structure of prolate ellipsoidal winds into a stationary ambient medium where both media can be either atomic or molecular. We specifically model the early twin-shock phase which generates a decelerating shell. A thick deformed and turbulent shell grows when an atomic wind expands into an atomic medium. In all other cases, the interaction shell region fragments into radial protrusions due to molecular cooling and chemistry. The resulting fingers eliminate any global slip parallel to the shell surface. This rough surface implies that weak shocks are prominent in the excitation of the gas despite the fast speed of advance. This may explain why low excitation molecular hydrogen is found towards the front of elliptical pPN. We constrain molecular dissociative fractions and timescales of fast H 2 winds and the pPN lifetime with wind densities ∼ 10 5 cm −3 and shock speeds of 80 ∼ 200 km s −1 . We identify a variety of stages associated with thermal excitation of H 2 near-infrared emission. Generated line emission maps and position-velocity diagrams enable a comparison and distinction with post-AGB survey results. The 1 → 0 S(1) & 2 → 1 S(1) lines are lobe-dominated bows rather than bipolar shells.

show abstract

“…The high-mass protostar S255IR NIRS 3 also seems to have a similar morphology, with variability in continuum and CO emission traced to light echoes (Caratti o Garatti et al 2017). This specific scenario, with H 2 emission from extended winds and CO emission produced by the disk but seen only in scattered light, also has a direct analog with the post-main sequence, pre-planetary nebula IRAS 16342-3814 (Gledhill & Forde 2012).…”

Section: Interpreting the Brightness Changes In The Infraredmentioning

confidence: 74%

Dissecting the different components of the modest accretion bursts of the very young protostar HOPS 373

Yoon,

Herczeg,

Lee

et al. 2022

Preprint

View full text Add to dashboard Cite

Observed changes in protostellar brightness can be complicated to interpret. In our JCMT Transient monitoring survey, we discovered that a young binary protostar, HOPS 373, is undergoing a modest 30% brightness increase at 850 µm, caused by a factor of 1.8-3.3 enhancement in the accretion rate. The initial burst occurred over a few months, with a sharp rise and then shallower decay. A second rise occurred soon after the decay, and the source is still bright one year later. The mid-IR emission, the small-scale CO outflow mapped with ALMA, and the location of variable maser emission indicate that the variability is associated with the SW component. The near-infrared and NEOWISE W 1 and W 2 emission is located along the blueshifted CO outflow, spatially offset by ∼ 3 to 4 from the SW component. The K-band emission imaged by UKIRT shows a compact H 2 emission source at the edge of the outflow, with a tail tracing the outflow back to the source. The W 1 emission, likely dominated by scattered light, brightens by 0.7 mag, consistent with expectations based on the sub-mm lightcurve. The signal of continuum variability in K-band and W 2 is masked by stable H 2 emission, as seen in our Gemini/GNIRS spectrum, and perhaps by CO emission. These differences in emission sources complicate infrared searches for variability of the youngest protostars.

show abstract

A fast bipolar H2 outflow from IRAS 16342−3814: an old star reliving its youth

Cited by 4 publications

References 63 publications

Dissecting the Different Components of the Modest Accretion Bursts of the Very Young Protostar HOPS 373

Dissecting the Different Components of the Modest Accretion Bursts of the Very Young Protostar HOPS 373

Numerical simulations of wind-driven protoplanetary nebulae – I. near-infrared emission

Dissecting the different components of the modest accretion bursts of the very young protostar HOPS 373

Contact Info

Product

Resources

About