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Journal articles on the topic 'Protostellar outflows'

Author: Grafiati

Published: 8 June 2024

Last updated: 31 July 2025

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1

Takaishi 髙石, Daisuke 大輔, Yusuke 裕介 Tsukamoto 塚本, Miyu 未宇 Kido 城戸, et al. "Formation of Unipolar Outflow and Protostellar Rocket Effect in Magnetized Turbulent Molecular Cloud Cores." Astrophysical Journal 963, no. 1 (2024): 20. http://dx.doi.org/10.3847/1538-4357/ad187a.

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Abstract Observed protostellar outflows exhibit a variety of asymmetrical features, including remarkable unipolar outflows and bending outflows. Revealing the formation and early evolution of such asymmetrical protostellar outflows, especially the unipolar outflows, is essential for a better understanding of the star and planet formation because they can dramatically change the mass accretion and angular momentum transport to the protostars and protoplanetary disks. Here we perform three-dimensional nonideal magnetohydrodynamics simulations to investigate the formation and early evolution of t

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Nakamura, Fumitaka, and Zhi-Yun Li. "Protostellar turbulence in cluster forming regions of molecular clouds." Proceedings of the International Astronomical Union 2, S237 (2006): 306–10. http://dx.doi.org/10.1017/s1743921307001640.

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AbstractWe perform 3D MHD simulations of cluster formation in turbulent magnetized dense molecular clumps, taking into account the effect of protostellar outflows. Our simulation shows that initial interstellar turbulence decays quickly as several authors already pointed out. When stars form, protostellar outflows generate and maintain supersonic turbulence that have a power-law energy spectrum of Ek ~ k−2, which is somewhat steeper than those of driven MHD turbulence simulations. Protostellar outflows suppress global star formation, although they can sometimes trigger local star formation by

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3

Skretas, I. M., and L. E. Kristensen. "Connecting Galactic and extragalactic outflows: From the Cygnus-X cluster to active galaxies." Astronomy & Astrophysics 660 (April 2022): A39. http://dx.doi.org/10.1051/0004-6361/202141944.

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Context. Molecular outflows are commonly detected originating from both protostellar and extragalactic sources. Separate studies of low-mass, isolated high-mass, and extragalactic sources reveal scaling relations connecting the force carried by an outflow and the properties of the source that drives it, as for example the mass and luminosity. Aims. The aim of this work is twofold: first, to examine the effects, if any, of clustered star formation on the protostellar outflows and their scaling relations and, second, to explore the possibility that outflows varying in scale and energetics by man

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4

Bally, John. "Protostellar Outflows." Annual Review of Astronomy and Astrophysics 54, no. 1 (2016): 491–528. http://dx.doi.org/10.1146/annurev-astro-081915-023341.

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Lin, Shuping. "Protostellar Outflows." Highlights in Science, Engineering and Technology 61 (July 30, 2023): 206–14. http://dx.doi.org/10.54097/hset.v61i.10297.

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The formation of massive stars differs from low-mass stars due to their rapid evolution, relatively low abundance, and their burial within molecular clouds, making observations more challenging. Moreover, the mechanisms give rise to the formation of O-type and B-type stars, in particular, differ from those responsible for the formation of low-mass stars. The paper presents an overview of the two main theories that have been proposed to explain the formation of massive stars: accretion and collision theories. The paper also investigates several mainstream theories of protostellar outflows durin

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6

Gómez-Ruiz, A. I., A. Gusdorf, S. Leurini, et al. "Warm gas in protostellar outflows." Astronomy & Astrophysics 629 (September 2019): A77. http://dx.doi.org/10.1051/0004-6361/201424156.

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Context. OMC-2/3 is one of the nearest embedded cluster-forming regions that includes intermediate-mass protostars at early stages of evolution. A previous CO (3–2) mapping survey towards this region revealed outflow activity related to sources at different evolutionary phases. Aims. The present work presents a study of the warm gas in the high-velocity emission from several outflows found in CO (3–2) emission by previous observations, determines their physical conditions, and makes a comparison with previous results in low-mass star-forming regions. Methods. We used the CHAMP+ heterodyne arra

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7

Nony, T., F. Motte, F. Louvet, et al. "Episodic accretion constrained by a rich cluster of outflows." Astronomy & Astrophysics 636 (April 2020): A38. http://dx.doi.org/10.1051/0004-6361/201937046.

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Context. The accretion history of protostars remains widely mysterious, even though it represents one of the best ways to understand the protostellar collapse that leads to the formation of stars. Aims. Molecular outflows, which are easier to detect than the direct accretion onto the prostellar embryo, are here used to characterize the protostellar accretion phase in W43-MM1. Methods. The W43-MM1 protocluster hosts a sufficient number of protostars to statistically investigate molecular outflows in a single, homogeneous region. We used the CO(2–1) and SiO(5–4) line datacubes, taken as part of

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8

Tokuda, Kazuki, Sarolta Zahorecz, Yuri Kunitoshi, et al. "The First Detection of a Protostellar CO Outflow in the Small Magellanic Cloud with ALMA." Astrophysical Journal Letters 936, no. 1 (2022): L6. http://dx.doi.org/10.3847/2041-8213/ac81c1.

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Abstract Protostellar outflows are one of the most outstanding features of star formation. Observational studies over the last several decades have successfully demonstrated that outflows are ubiquitously associated with low- and high-mass protostars in solar-metallicity Galactic conditions. However, the environmental dependence of protostellar outflow properties is still poorly understood, particularly in the low-metallicity regime. Here we report the first detection of a molecular outflow in the Small Magellanic Cloud with 0.2 Z ⊙, using Atacama Large Millimeter/submillimeter Array observati

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Rohde, P. F., S. Walch, D. Seifried, A. P. Whitworth, and S. D. Clarke. "Protostellar outflows: a window to the past." Monthly Notices of the Royal Astronomical Society 510, no. 2 (2021): 2552–71. http://dx.doi.org/10.1093/mnras/stab3572.

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ABSTRACT During the early phases of low-mass star formation, episodic accretion causes the ejection of high-velocity outflow bullets, which carry a fossil record of the driving protostar’s accretion history. We present 44 SPH simulations of $1\, {{\mathrm{M}}}_{\odot }$ cores, covering a wide range of initial conditions, and follow the cores for five free-fall times. Individual protostars are represented by sink particles, and the sink particles launch episodic outflows using a sub-grid model. The Optics algorithm is used to identify individual episodic bullets within the outflows. The paramet

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Myers, Philip C., Michael M. Dunham, and Ian W. Stephens. "Can Protostellar Outflows Set Stellar Masses?" Astrophysical Journal 949, no. 1 (2023): 19. http://dx.doi.org/10.3847/1538-4357/acca74.

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Abstract 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 magneti

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11

Duffin, Dennis F., and Ralph E. Pudritz. "Discs, outflows, and feedback in collapsing magnetized cores." Proceedings of the International Astronomical Union 6, S270 (2010): 291–95. http://dx.doi.org/10.1017/s1743921311000536.

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AbstractThe pre-stellar cores in which low mass stars form are generally well magnetized. Our simulations show that early protostellar discs are massive and experience strong magnetic torques in the form of magnetic braking and protostellar outflows. Simulations of protostellar disk formation suggest that these torques are strong enough to suppress a rotationally supported structure from forming for near critical values of mass-to-flux. We demonstrate through the use of a 3D adaptive mesh refinement code – including cooling, sink particles and magnetic fields – that one produces transient 1000

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12

Walawender, Josh, Grace Wolf-Chase, Michael Smutko, JoAnn OLinger-Luscusk, and Gerald Moriarty-Schieven. "PROTOSTELLAR OUTFLOWS IN L1340." Astrophysical Journal 832, no. 2 (2016): 184. http://dx.doi.org/10.3847/0004-637x/832/2/184.

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13

Froebrich, Dirk, Michael D. Smith, and Jochen Eislöffel. "Shocks in Protostellar Outflows." Astrophysics and Space Science 287, no. 1-4 (2003): 217–20. http://dx.doi.org/10.1023/b:astr.0000006227.85806.85.

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14

Mignon-Risse, R., M. González, and B. Commerçon. "Collapse of turbulent massive cores with ambipolar diffusion and hybrid radiative transfer." Astronomy & Astrophysics 656 (December 2021): A85. http://dx.doi.org/10.1051/0004-6361/202141648.

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Context. Most massive protostars exhibit bipolar outflows. Nonetheless, there is no consensus regarding the mechanism at the origin of these outflows, nor on the cause of the less-frequently observed monopolar outflows. Aims. We aim to identify the origin of early massive protostellar outflows, focusing on the combined effects of radiative transfer and magnetic fields in a turbulent medium. Methods. We use four state-of-the-art radiation-magnetohydrodynamical simulations following the collapse of massive 100 M⊙ pre-stellar cores with the RAMSES code. Turbulence is taken into account via initia

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15

Xu, Duo, Stella S. R. Offner, Robert Gutermuth, Shuo Kong, and Hector G. Arce. "A Census of Protostellar Outflows in Nearby Molecular Clouds." Astrophysical Journal 926, no. 1 (2022): 19. http://dx.doi.org/10.3847/1538-4357/ac39a0.

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Abstract We adopt the deep learning method casi-3d (Convolutional Approach to Structure Identification-3D) to systemically identify protostellar outflows in 12CO and 13CO observations of the nearby molecular clouds, Ophiuchus, Taurus, Perseus, and Orion. The total outflow masses are 267 M ⊙, 795 M ⊙, 1305 M ⊙, and 6332 M ⊙ for Ophiuchus, Taurus, Perseus, and Orion, respectively. We show the outflow mass in each cloud is linearly proportional to the total number of young stellar objects. The estimated total 3D deprojected outflow energies are 9 × 1045 erg, 6 × 1046 erg, 1.2 × 1047 erg, and 6 ×

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Machida, Masahiro N., and Takashi Hosokawa. "Failed and delayed protostellar outflows with high-mass accretion rates." Monthly Notices of the Royal Astronomical Society 499, no. 3 (2020): 4490–514. http://dx.doi.org/10.1093/mnras/staa3139.

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ABSTRACT The evolution of protostellar outflows is investigated under different mass accretion rates in the range ∼10−5–$10^{-2}\, {\rm M}_\odot$ yr−1 with 3D magnetohydrodynamic simulations. A powerful outflow always appears in strongly magnetized clouds with $B_0 \gtrsim B_{\rm 0, cr}\, =10^{-4} (M_{\rm cl}/100\, {\rm M}_\odot)$ G, where Mcl is the cloud mass. When a cloud has a weaker magnetic field, the outflow does not evolve promptly with a high-mass accretion rate. In some cases with moderate magnetic fields B0 slightly smaller than B0, cr, the outflow growth is suppressed or delayed un

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17

Sperling, T., J. Eislöffel, C. Fischer, B. Nisini, T. Giannini, and A. Krabbe. "Evolution of the atomic component in protostellar outflows." Astronomy & Astrophysics 650 (June 2021): A173. http://dx.doi.org/10.1051/0004-6361/202040048.

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Context. We present SOFIA/FIFI-LS observations of three Class 0 and one Class I outflows (Cep E, HH 1, HH 212, and L1551 IRS5) in the far-infrared [O I]63 μm and [O I]145 μm transitions. Spectroscopic [O I]63 μm maps enabled us to infer the spatial extent of warm (T ∼ 500−1200 K), low-excitation atomic gas within these protostellar outflows. Aims. Our main goal is to determine mass-loss rates from the obtained [OI]63 μm maps and compare these with accretion rates from other studies. Methods. The far-infrared [O I]63 μm emission line is predicted to be the main coolant of dense, dissociative J-

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18

Gomez-Ruiz, A. I., F. Wyrowski, A. Gusdorf, S. Leurini, K. M. Menten, and R. Güsten. "Warm gas in protostellar outflows." Astronomy & Astrophysics 555 (June 19, 2013): A8. http://dx.doi.org/10.1051/0004-6361/201218824.

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19

Fukui, Y., T. Iwata, H. Takaba, et al. "Molecular outflows in protostellar evolution." Nature 342, no. 6246 (1989): 161–63. http://dx.doi.org/10.1038/342161a0.

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20

Zapata, Luis A., Johannes Schmid-Burgk, Luis F. Rodríguez, Aina Palau, and Laurent Loinard. "Molecular Outflows: Explosive versus Protostellar." Astrophysical Journal 836, no. 1 (2017): 133. http://dx.doi.org/10.3847/1538-4357/aa5b94.

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21

Hsieh, Cheng-Han, Héctor G. Arce, Zhi-Yun Li, et al. "The Evolution of Protostellar Outflow Cavities, Kinematics, and Angular Distribution of Momentum and Energy in Orion A: Evidence for Dynamical Cores." Astrophysical Journal 947, no. 1 (2023): 25. http://dx.doi.org/10.3847/1538-4357/acba13.

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Abstract We present Atacama Large Millimeter/submillimeter Array observations of the ∼10,000 au environment surrounding 21 protostars in the Orion A molecular cloud tracing outflows. Our sample is composed of Class 0 to flat-spectrum protostars, spanning the full ∼1 Myr lifetime. We derive the angular distribution of outflow momentum and energy profiles and obtain the first two-dimensional instantaneous mass, momentum, and energy ejection rate maps using our new approach: the pixel flux-tracing technique. Our results indicate that by the end of the protostellar phase, outflows will remove ∼2–4

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22

Arce, Héctor G. "Outflow-Circumstellar Envelope Interactions in Protostars." Symposium - International Astronomical Union 221 (2004): 345–50. http://dx.doi.org/10.1017/s0074180900241764.

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We present the results of a high angular resolution (< 5″) survey of protostars with outflows, at different evolutionary stages, using the Owens Valley Radio Observatory Millimeter Array. This survey aims to understand the evolution of the interaction between protostellar outflows and the infalling circumstellar envelopes. Our data enable us to probe the structure and kinematics of the molecular outflow and the circumstellar envelope, as well as the outflow-envelope interaction at scales of less than 0.02 pc, for every source in our sample. Our results indicate that outflows have a consider

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23

Kuiper, R., and T. Hosokawa. "First hydrodynamics simulations of radiation forces and photoionization feedback in massive star formation." Astronomy & Astrophysics 616 (August 2018): A101. http://dx.doi.org/10.1051/0004-6361/201832638.

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Aims. We present the first simulations of the formation and feedback of massive stars which account for radiation forces as well as photoionization feedback (along with protostellar outflows). In two different accretion scenarios modeled, we determine the relative strength of these feedback components and derive the size of the reservoir from which the forming stars gained their masses. Methods. We performed direct hydrodynamics simulations of the gravitational collapse of high-density mass reservoirs toward the formation of massive stars including self-gravity, stellar evolution, protostellar

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Lora, V., T. Nony, A. Esquivel, and R. Galván-Madrid. "Shedding Light on the Ejection History of Molecular Outflows: Multiple Velocity Modes and Precession." Astrophysical Journal 962, no. 1 (2024): 66. http://dx.doi.org/10.3847/1538-4357/ad13ed.

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Abstract Variable accretion has been well studied in the evolved stages of low-mass star formation. However, the accretion history in the initial phases of star formation is still a seldom studied topic. The outflows and jets emerging from protostellar objects could shed some light on their accretion history. We consider the recently studied case of W43-MM1, a protocluster containing 46 outflows driven by 27 protostellar cores. The outflow kinematics of the individual cores and associated knots in W43-MM1 indicate episodic protostellar ejection. We take the observed parameters of an individual

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FRANK, ADAM. "PROTOSTELLAR OUTFLOWS: NEW PERSPECTIVES ON MESOSCOPIC STRUCTURE AND MACROSCOPIC FEEDBACK." Modern Physics Letters A 24, no. 15 (2009): 1167–85. http://dx.doi.org/10.1142/s0217732309030989.

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This paper presents a brief review of new perspectives in the field of protostellar outflows concentrating on scales above those associated with the launch region (L > 10 AU ). The formation and propagation of protostellar or Young Stellar Object (YSO) jets and collimated outflows has been intensively studied over the last 30 years with enormous progress being made in both theory and observations. As both the resolution and integration of observational platforms increases new features are revealed which have shifted the emphasis of research efforts. In this paper we review results in two di

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Frank, A. "Hypersonic Swizzle Sticks: Protostellar Turbulence, Outflows and Fossil Outflow Cavities." Astrophysics and Space Science 307, no. 1-3 (2007): 35–39. http://dx.doi.org/10.1007/s10509-006-9283-9.

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Li, Guang-Xing, Keping Qiu, Friedrich Wyrowski, and Karl Menten. "Turbulent entrainment origin of protostellar outflows." Astronomy & Astrophysics 559 (October 30, 2013): A23. http://dx.doi.org/10.1051/0004-6361/201220581.

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Nisini, B., G. Santangelo, S. Antoniucci, et al. "Mapping water in protostellar outflows withHerschel." Astronomy & Astrophysics 549 (December 6, 2012): A16. http://dx.doi.org/10.1051/0004-6361/201220163.

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29

Contopoulos, I., and C. Sauty. "The origin of molecular protostellar outflows." Astronomy & Astrophysics 365, no. 2 (2001): 165–73. http://dx.doi.org/10.1051/0004-6361:20000329.

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30

Nakamura, Fumitaka, and Zhi‐Yun Li. "Protostellar Turbulence Driven by Collimated Outflows." Astrophysical Journal 662, no. 1 (2007): 395–412. http://dx.doi.org/10.1086/517515.

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31

Rawlings, J. M. C., J. E. Drew, and M. J. Barlow. "Excited Hydrogen Chemistry in Protostellar Outflows." Symposium - International Astronomical Union 150 (1992): 387–88. http://dx.doi.org/10.1017/s0074180900090446.

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Chemical models of protostellar and other outflows have been reassessed in the light of new chemical data. In particular, reactions involving excited hydrogen (2s,p) are shown to be important in hot, dense outflows. The H(n=2) + H → H2 + hv reaction is much less of a contributor to the H2 formation rate than the recently measured H(n=2) + H → H2+ + e- reaction, providing conditions allow the 0.75eV endothermicity of this reaction to be overcome.

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Bürzle, Florian, Paul C. Clark, Federico Stasyszyn, Klaus Dolag, and Ralf S. Klessen. "Protostellar outflows with smoothed particle magnetohydrodynamics." Monthly Notices of the Royal Astronomical Society: Letters 417, no. 1 (2011): L61—L65. http://dx.doi.org/10.1111/j.1745-3933.2011.01120.x.

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33

Dutta, Somnath, Chin-Fei Lee, Naomi Hirano, et al. "ALMA Survey of Orion Planck Galactic Cold Clumps (ALMASOP): Evidence for a Molecular Jet Launched at an Unprecedented Early Phase of Protostellar Evolution." Astrophysical Journal 931, no. 2 (2022): 130. http://dx.doi.org/10.3847/1538-4357/ac67a1.

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Abstract Protostellar outflows and jets play a vital role in star formation as they carry away excess angular momentum from the inner disk surface, allowing the material to be transferred toward the central protostar. Theoretically, low-velocity and poorly collimated outflows appear from the beginning of the collapse at the first hydrostatic core (FHSC) stage. With growing protostellar core mass, high-density jets are launched, entraining an outflow from the infalling envelope. Until now, molecular jets have been observed at high velocity (≳100 km s−1) in early Class 0 protostars. We, for the

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Podio, Linda, Benoit Tabone, and Claudio Codella. "Protostellar jets: A statistical view with the CALYPSO IRAM-PdBI survey." EPJ Web of Conferences 265 (2022): 00037. http://dx.doi.org/10.1051/epjconf/202226500037.

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In the context of the CALYPSO IRAM-PdBI Lai•ge Program we performed the first statistical survey of protostellar jets by analysing molecular emission in a sample of 21 protostars covering a broad range of internal luminosities (Lint from 0.035 L⊙ to 47 L⊙). We find that the outflow phenomenon is ubiquitous in our sample of protostars, with wide-angle outflows detected in CO (2 - 1) in all sources, and high-velocity collimated jets detected in SiO (5-4) in 80% of the sources with Lint > 1 L⊙. The protostellar flows have an onion-like structure, with the SiO jet (opening angle, α ~ 10°) neste

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Lee, Seokho, Jeong-Eun Lee, Doug Johnstone, Gregory J. Herczeg, and Yuri Aikawa. "Multiple Jets in the Bursting Protostar HOPS 373SW." Astrophysical Journal 964, no. 1 (2024): 34. http://dx.doi.org/10.3847/1538-4357/ad21e3.

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Abstract We present the outflows detected in HOPS 373SW, a protostar undergoing a modest 30% brightness increase at 850 μm. Atacama Large Millimeter/submillimeter Array observations of shock tracers, including SiO 8–7, CH3OH 7k–6k, and 12CO 3–2 emission, reveal several outflow features around HOPS 373SW. The knots in the extremely high-velocity SiO emission reveal the wiggle of the jet, for which a simple model derives a 37° inclination angle of the jet to the plane of the sky, a jet velocity of 90 km s−1, and a period of 50 yr. The slow SiO and CH3OH emission traces U-shaped bow shocks surrou

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Moscadelli, L., A. Sanna, C. Goddi, V. Krishnan, F. Massi, and F. Bacciotti. "Protostellar Outflows at the EarliesT Stages (POETS)." Astronomy & Astrophysics 631 (October 22, 2019): A74. http://dx.doi.org/10.1051/0004-6361/201936436.

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Context. Although recent observations and theoretical simulations have pointed out that accretion disks and jets can be essential for the formation of stars with a mass of up to at least 20 M⊙, the processes regulating mass accretion and ejection are still uncertain. Aims. The goal of the Protostellar Outflows at the EarliesT Stages (POETS) survey is to image the disk-outflow interface on scales of 10–100 au in a statistically significant sample (36) of luminous young stellar objects (YSO), targeting both the molecular and ionized components of the outflows. Methods. The outflow kinematics is

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Thieme, Travis J., Shih-Ping Lai, Sheng-Jun Lin, et al. "Accretion Flows or Outflow Cavities? Uncovering the Gas Dynamics around Lupus 3-MMS." Astrophysical Journal 925, no. 1 (2022): 32. http://dx.doi.org/10.3847/1538-4357/ac382b.

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Abstract Understanding how material accretes onto the rotationally supported disk from the surrounding envelope of gas and dust in the youngest protostellar systems is important for describing how disks are formed. Magnetohydrodynamic simulations of magnetized, turbulent disk formation usually show spiral-like streams of material (accretion flows) connecting the envelope to the disk. However, accretion flows in these early stages of protostellar formation still remain poorly characterized, due to their low intensity, and possibly some extended structures are disregarded as being part of the ou

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Arce, Héctor G. "Outflows and Turbulence in Young Stellar Clusters — An Observer's View." Proceedings of the International Astronomical Union 6, S270 (2010): 287–90. http://dx.doi.org/10.1017/s1743921311000524.

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AbstractRecent numerical studies have focused their interest on the impact outflows have on the cloud's turbulence. The contradictory results obtained by these studies indicate that it is essential for observers to provide the required data to constrain the models. Here we discuss the impact of outflows on the environment surrounding clusters of young stellar objects, from an observer's point of view. We have conducted several studies of outflows in different active star-forming regions. In all cases it is clear that outflows have the power to sustain the observed turbulence in the gas surroun

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Pudritz, Ralph E., and Colin A. Norman. "Hydromagnetic winds from accretion disks." Canadian Journal of Physics 64, no. 4 (1986): 501–6. http://dx.doi.org/10.1139/p86-094.

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We present a hydromagnetic wind model for molecular and ionized gas outflows associated with protostars. If the luminosity of protostars is due to accretion, then centrifugally driven winds that arise from the envelopes of molecular disks explain the observed rates of momentum and energy transport. Ionized outflow originates from disk radii r ≤ 1015 cm inside of which Ly-continuum photons from the protostellar accretion shock are intercepted. Observed molecular outflows arise from the cool disk envelope at radii 1015 ≤ r ≤ 1017 cm. The mass-loss rates of these two component outflows are [Formu

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Green, Joel D., Klaus M. Pontoppidan, Megan Reiter, et al. "Why Are (Almost) All the Protostellar Outflows Aligned in Serpens Main?" Astrophysical Journal 972, no. 1 (2024): 5. http://dx.doi.org/10.3847/1538-4357/ad5a02.

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Abstract We present deep 1.4–4.8 μm JWST-NIRCam imaging of the Serpens Main star-forming region and identify 20 candidate protostellar outflows, most with bipolar structure and identified driving sources. The outflow position angles (PAs) are strongly correlated, and they are aligned within ±24° of the major axis of the Serpens filament. These orientations are further aligned with the angular momentum vectors of the two disk shadows in this region. We estimate that the probability of this number of young stars being coaligned if sampled from a uniform PA distribution is 10−4. This in turn sugg

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Sanna, A., L. Moscadelli, C. Goddi, et al. "Protostellar Outflows at the EarliesT Stages (POETS)." Astronomy & Astrophysics 623 (March 2019): L3. http://dx.doi.org/10.1051/0004-6361/201834551.

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Centimeter continuum observations of protostellar jets have revealed knots of shocked gas where the flux density decreases with frequency. This spectrum is characteristic of nonthermal synchrotron radiation and implies both magnetic fields and relativistic electrons in protostellar jets. Here, we report on one of the few detections of a nonthermal jet driven by a young massive star in the star-forming region G035.02+0.35. We made use of the NSF’s Karl G. Jansky Very Large Array (VLA) to observe this region at C, Ku, and K bands with the A- and B-array configurations, and obtained sensitive rad

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Stephens, Ian W., Michael M. Dunham, Philip C. Myers, et al. "Alignment between Protostellar Outflows and Filamentary Structure." Astrophysical Journal 846, no. 1 (2017): 16. http://dx.doi.org/10.3847/1538-4357/aa8262.

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Nisini, B., M. Benedettini, C. Codella, et al. "Water cooling of shocks in protostellar outflows." Astronomy and Astrophysics 518 (July 2010): L120. http://dx.doi.org/10.1051/0004-6361/201014603.

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Krumholz, Mark R., Christopher F. McKee, and Richard I. Klein. "How Protostellar Outflows Help Massive Stars Form." Astrophysical Journal 618, no. 1 (2004): L33—L36. http://dx.doi.org/10.1086/427555.

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Machida, Masahiro N. "PROTOSTELLAR JETS ENCLOSED BY LOW-VELOCITY OUTFLOWS." Astrophysical Journal 796, no. 1 (2014): L17. http://dx.doi.org/10.1088/2041-8205/796/1/l17.

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Sanna, A., L. Moscadelli, C. Goddi, V. Krishnan, and F. Massi. "Protostellar Outflows at the EarliesT Stages (POETS)." Astronomy & Astrophysics 619 (November 2018): A107. http://dx.doi.org/10.1051/0004-6361/201833573.

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Context. Weak and compact radio continuum and H2O masers are preferred tracers of the outflow activity nearby very young stars. Aims. We want to image the centimeter free–free continuum emission in the range 1–7 cm (26–4 GHz), which arises in the inner few 1000 au from those young stars also associated with bright H2O masers. We seek to study the radio continuum properties in combination with the H2O maser kinematics to quantify the outflow energetics powered by single young stars. Methods. We made use of the Karl G. Jansky Very Large Array (VLA) in the B configuration at K band and the A conf

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Peters, Thomas, Pamela D. Klaassen, Daniel Seifried, Robi Banerjee, and Ralf S. Klessen. "Morphologies of protostellar outflows: an ALMA view." Monthly Notices of the Royal Astronomical Society 437, no. 3 (2013): 2901–8. http://dx.doi.org/10.1093/mnras/stt2104.

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Moscadelli, L., A. Sanna, C. Goddi, V. Krishnan, F. Massi, and F. Bacciotti. "Protostellar Outflows at the EarliesT Stages (POETS)." Astronomy & Astrophysics 635 (March 2020): A118. http://dx.doi.org/10.1051/0004-6361/202037472.

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Context. 22 GHz water masers are the most intense and widespread masers in star-forming regions. They are commonly associated with protostellar winds and jets emerging from low- and high-mass young stellar objects (YSO). Aims. We wish to perform for the first time a statistical study of the location and motion of individual water maser cloudlets, characterized by typical sizes that are within a few au, with respect to the weak radio thermal emission from YSOs. Methods. For this purpose, we have been carrying out the Protostellar Outflows at the EarliesT Stages survey of a sample (38) of high-m

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Shu, Frank H., and Hsien Shang. "Protostellar X-Rays, Jets, and Bipolar Outflows." Symposium - International Astronomical Union 182 (1997): 225–39. http://dx.doi.org/10.1017/s0074180900061672.

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We review the theory of x-winds in young stellar objects (YSOs). In particular, we consider how a model where the central star does not corotate with the inner edge of the accretion disk may help to explain the enhanced emission of X-rays from embedded protostars. We argue, however, that the departure from corotation is not large, so a mathematical formulation that treats the long-term average state as steady and axisymmetric represents a useful approximation. Magnetocentrifugally driven x-winds of this description collimate into jets, and their interactions with the surrounding molecular clou

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Rosen, A., and M. D. Smith. "Numerical simulations of highly collimated protostellar outflows." Astronomy & Astrophysics 413, no. 2 (2003): 593–607. http://dx.doi.org/10.1051/0004-6361:20031566.

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