Models of Rotating Infall for the B335 Protostar

Evans, Neal J.; Yang, Yao-Lun; Green, Joel D.; Zhao, Bo; Francesco, James Di; Lee, Jeong Eun; Jørgensen, J. K.; Choi, Minho; Myers, Philip C.; Mardones, Diego

doi:10.3847/1538-4357/acaa38

Cited by 14 publications

(19 citation statements)

References 69 publications

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“…According to this relation, the outburst luminosity at MJD 58391 is enhanced by a factor of ∼5 over the quiescent luminosity at MJD 55304. This result is consistent with the luminosity calculated using the relation found in Evans et al (2023). Therefore, we adopt the relation between the W2 flux density and central luminosity of B335 by Evans et al (2023) to calculate the variation of the central luminosity over the recent burst.…”

Section: Mass Ratio Between Ejection and Accretionsupporting

confidence: 88%

“…We convert the W2 magnitude into the W2 flux density (see the right y-axis in Figure 1) as a proxy for the central luminosity. The relation between the central luminosity and the W2 flux density of B335 has been explored based on the 3D continuum modeling by Evans et al (2023);…”

Section: Mass Ratio Between Ejection and Accretionmentioning

confidence: 99%

“…To calculate the mass accretion rate, we need some additional properties of B335 (R å , M å , and f acc = 0.5). In the 3D continuum modeling explored by Evans et al (2023), the luminosity depends upon R å and the temperature, T å , of the source. Evans et al (2023) held fixed T å and varied R å to match the observed quiescent luminosity, which is the spectral energy distribution (SED) modeling result using various photometric data observed before MJD 57000.…”

Section: Mass Ratio Between Ejection and Accretionmentioning

confidence: 99%

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The CO Outflow Components Ejected by a Recent Accretion Event in B335

Kim,

Lee,

Peña

et al. 2024

ApJ

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Protostellar outflows often present a knotty appearance, providing evidence of sporadic accretion in stellar mass growth. To understand the direct relation between mass accretion and ejection, we analyze the contemporaneous accretion activity and associated ejection components in B335. B335 has brightened in the mid-IR by 2.5 mag since 2010, indicating increased luminosity, presumably due to an increased mass accretion rate onto the protostar. Atacama Large Millimeter/submillimeter Array (ALMA) observations of 12CO emission in the outflow reveal high-velocity emission, estimated to have been ejected 4.6–2 yr before the ALMA observations and consistent with the jump in mid-IR brightness. The consistency in timing suggests that the detected high-velocity ejection components are directly linked to the most recent accretion activity. We calculated the kinetic energy, momentum, and force for the ejection component associated with the most recent accretion activity and found that, at least, about 1.0% of the accreted mass has been ejected. More accurate information on the jet inclination and the temperature of the ejected gas components will better constrain the ejected mass induced by the recently enhanced accretion event.

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Section: Mass Ratio Between Ejection and Accretionsupporting

confidence: 88%

Section: Mass Ratio Between Ejection and Accretionmentioning

confidence: 99%

Section: Mass Ratio Between Ejection and Accretionmentioning

confidence: 99%

See 1 more Smart Citation

The CO Outflow Components Ejected by a Recent Accretion Event in B335

Kim,

Lee,

Peña

et al. 2024

ApJ

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“…A model based on a rotating, collapsing SIS (Terebey et al 1984) was developed to match line and continuum observations of the protostellar core B335 (Evans et al 2023). The best-fit velocity dispersion, collapse age, and protostar mass are similar to those modeled here, while the envelope outer radius is greater by a factor ∼3.…”

Section: Comparison To Similar Studiesmentioning

confidence: 69%

Can Protostellar Outflows Set Stellar Masses?

Myers

Dunham

Stephens

2023

ApJ

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The opening angles of some protostellar outflows appear too narrow to match the expected core–star mass efficiency (SFE) = 0.3–0.5, if the outflow cavity volume traces outflow mass, with a conical shape and a maximum opening angle near 90°. However, outflow cavities with a paraboloidal shape and wider angles are more consistent with observed estimates of the SFE. This paper presents a model of infall and outflow evolution based on these properties. The initial state is a truncated singular isothermal sphere which has mass ≈ 1 M ⊙, freefall time ≈ 80 kyr, and small fractions of magnetic, rotational, and turbulent energy. The core collapses pressure free as its protostar and disk launch a paraboloidal wide-angle wind. The cavity walls expand radially and entrain envelope gas into the outflow. The model matches the SFE values when the outflow mass increases faster than the protostar mass by a factor 1–2, yielding protostar masses typical of the IMF. It matches the observed outflow angles if the outflow mass increases at nearly the same rate as the cavity volume. The predicted outflow angles are then typically ∼50° as they increase rapidly through the stage 0 duration of ∼40 kyr. They increase more slowly up to ∼110° during their stage I duration of ∼70 kyr. With these outflow rates and shapes, the model predictions appear consistent with observational estimates of the typical stellar masses, SFEs, stage durations, and outflow angles, with no need for external mechanisms of core dispersal.

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“…Jacobsen et al (2019) attributed this emission to the innermost warm envelope. B335, in Bok globule B335, has a relatively low bolometric luminosity (L bol = 1.36 L e ), and the COM distribution remains unresolved at a scale of ∼45 au (or HPBW = 0 55 at a distance d ∼ 165 pc; Hirano et al 1988;Yen et al 2010;Imai et al 2016;Watson 2020;Evans & Yang 2023). There exist luminosity variations in B335 (Evans & Yang 2023), which have admittedly led to variations in the warm region size.…”

Section: The Luminosity and Radius Of The Com Extentmentioning

confidence: 99%

ALMA Survey of Orion Planck Galactic Cold Clumps (ALMASOP): The Warm-envelope Origin of Hot Corinos

Hsu,

Liu,

Johnstone

et al. 2023

ApJ

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Hot corinos are of great interest due to their richness in interstellar complex organic molecules (COMs) and the consequent potential prebiotic connection to solar-like planetary systems. Recent surveys have reported an increasing number of detected hot corinos in Class 0/I protostars; however, the relationships between their physical properties and the hot-corino signatures remain elusive. In this study, our objective is to establish a general picture of the detectability of hot corinos by identifying the origins of the hot-corino signatures in the sample of young stellar objects (YSOs) obtained from the Atacama Large Millimeter/submillimeter Array Survey of Orion Planck Galactic Cold Clumps project. We apply spectral energy distribution modeling to our sample and identify the physical parameters of the modeled YSOs directly, linking the detection of hot-corino signatures to the envelope properties of the YSOs. Imaging simulations of the methanol emission further support this scenario. We therefore posit that the observed COM emission originates from the warm inner envelopes of the sample YSOs, based on both the warm region size and the envelope density profile. The former is governed by the source luminosity and is additionally affected by the disk and cavity properties, while the latter is related to the evolutionary stages. This scenario provides a framework for detecting hot-corino signatures toward luminous Class 0 YSOs, with fewer detections being observed toward similarly luminous Class I sources.

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Models of Rotating Infall for the B335 Protostar

Cited by 14 publications

References 69 publications

The CO Outflow Components Ejected by a Recent Accretion Event in B335

The CO Outflow Components Ejected by a Recent Accretion Event in B335

Can Protostellar Outflows Set Stellar Masses?

ALMA Survey of Orion Planck Galactic Cold Clumps (ALMASOP): The Warm-envelope Origin of Hot Corinos

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