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5 results on '"DG-TAURI"'

1. X-ray emission from stellar jets by collision against high-density molecular clouds: an application to HH 248

Author

López Santiago, J., Bonito, R., Orellana, M., Miceli, M., Orlando, S., Ustamujic, S., Albacete Colombo, J. F., Castro Rubio, Elisa de, Gómez de Castro, Ana Inés, López Santiago, J., Bonito, R., Orellana, M., Miceli, M., Orlando, S., Ustamujic, S., Albacete Colombo, J. F., Castro Rubio, Elisa de, and Gómez de Castro, Ana Inés

Abstract

© 2015. The American Astronomical Society. The software used in this work was developed in part by the DOE-supported ASC/Alliance Center for Astrophysical Thermonuclear Flashes at the University of Chicago. HST data presented in this paper were obtained from MAST. STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NNX13AC07G and by other grants and contracts. This work was supported by the Spanish Government under research projects AYA2011-29754-C03-01 and AYA2011-29754-C03-03. M.O. and J.F.A-C. acknowledge support by the Consejo Nacional de Investigaciones Científicas y Técnicas (CONICET, Argentina). Finally, we thank the referee for useful comments and suggestions., We investigate the plausibility of detecting X-ray emission from a stellar jet that impacts a dense molecular cloud, a scenario that may be typical for classical T Tauri stars with jets in dense star-forming complexes. We first model the impact of a jet against a dense cloud using two-dimensional axisymmetric hydrodynamic simulations, exploring different configurations of the ambient environment. Then, we compare our results with XMM-Newton observations of the Herbig-Haro object HH 248, where extended X-ray emission aligned with the optical knots is detected at the edge of the nearby IC 434 cloud. Our simulations show that a jet can produce plasma with temperatures up to 10^7 K, consistent with production of X-ray emission, after impacting a dense cloud. We find that jets denser than the ambient medium but less dense than the cloud produce detectable X-ray emission only at impact with the cloud. From an exploration of the model parameter space, we constrain the physical conditions (jet density and velocity and cloud density) that reproduce the intrinsic luminosity and emission measure of the X-ray source possibly associated with HH 248 well. Thus, we suggest that the extended X-ray source close to HH 248 corresponds to a jet impacting a dense cloud., National Aeronautics and Spacial Agency (NASA), EE.UU, Gobierno de España, Consejo Nacional de Investigaciones Científicas y Técnicas (CONICET, Argentina), DOE-supported ASC/Alliance Center for Astrophysical Thermonuclear Flashes, University of Chicago (EE.UU), Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

Published
2023

2. Evidence of non-thermal x-ray emission from HH 80

Author

López Santiago, Javier, Peri, C. S., Bonito, R., Miceli, M., Albacete Colombo, J. F., Benaglia, P., Castro Rubio, Elisa de, López Santiago, Javier, Peri, C. S., Bonito, R., Miceli, M., Albacete Colombo, J. F., Benaglia, P., and Castro Rubio, Elisa de

Abstract

© 2013. The American Astronomical Society. This work was supported by the Spanish Government (AYA2011-29754-C03-01 and AYA2011-29754-C03-03). C. S. P. was supported by the COSPAR Capacity Building Workshop Fellowship Program and the Universidad Nacional de La Plata to develop this work at the Universidad Complutense de Madrid. M. M. is supported through the ASI-INAF contract I/009/10/0. JFAC is a staff researcher of the CONICET and acknowledges support by grant PIP 2011 0100285. J.L.-S. would like to thank Drs. F. J. Carrera, P. G. Pérez González and S. Mateos for fruitful discussion on the spectral X-ray emission properties of AGN. We also acknowledges the referee of this manuscript for their suggestions and comments. Facilities: XMM-Newton (EPIC), Chandra (ACIS), Spitzer (IRAC, MIPS)., Protostellar jets appear at all stages of star formation when the accretion process is still at work. Jets travel at velocities of hundreds of km s^-1, creating strong shocks when interacting with the interstellar medium. Several cases of jets have been detected in X-rays, typically showing soft emission. For the first time, we report evidence of hard X-ray emission possibly related to non-thermal processes not explained by previous models of the post-shock emission predicted in the jet/ambient interaction scenario. HH 80 is located at the south head of the jet associated with the massive protostar IRAS 18162-2048. It shows soft and hard X-ray emission in regions that are spatially separated, with the soft X-ray emission region situated behind the region of hard X-ray emission. We propose a scenario for HH 80 where soft X-ray emission is associated with thermal processes from the interaction of the jet with denser ambient matter and hard X-ray emission is produced by synchrotron radiation at the front shock., Ministerio de Ciencia e Innovación (MCINN), España, Agenzia Spaziale Italiana (ASI), Istituto Nazionale di Astrofisica (INAF), Universidad Nacional de La Plata, Consejo Nacional de Investigaciones Científicas y Técnicas (CONICET), Argentina, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

Published
2023

3. Laboratory formation of a scaled protostellar jet by coaligned poloidal magnetic field

Author

Hans-Peter Schlenvoigt, G. Revet, Marco Borghesi, Martín Huarte-Espinosa, I. Yu. Skobelev, Henri Pépin, K. Naughton, Motoaki Nakatsutsumi, O. Portugall, Andrea Ciardi, J. Béard, T. Herrmannsdörfer, Zakary Burkley, Thomas E. Cowan, Julien Fuchs, S. A. Pikuz, Florian Kroll, Tommaso Vinci, R. Riquier, A. Ya. Faenov, A. A. Soloviev, Rosaria Bonito, Caterina Riconda, L. Romagnani, Adam Frank, Drew Higginson, J. Billette, Bruno Albertazzi, Sophia Chen, Laboratoire pour l'utilisation des lasers intenses (LULI), Université Pierre et Marie Curie - Paris 6 (UPMC)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Laboratoire national des champs magnétiques intenses - Toulouse (LNCMI-T), Institut National des Sciences Appliquées - Toulouse (INSA Toulouse), Institut National des Sciences Appliquées (INSA)-Université de Toulouse (UT)-Institut National des Sciences Appliquées (INSA)-Université de Toulouse (UT)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Albertazzi, B., Ciardi, A., Nakatsutsumi, M., Vinci, T., Béard, J., Bonito, R., Billette, J., Borghesi, M., Burkley, Z., Chen, S. N., Cowan, T. E., Herrmannsdörfer, T., Higginson, D. P., Kroll, F., Pikuz, S. A., Naughton, K., Romagnani, L., Riconda, C., Revet, G., Riquier, R., Schlenvoigt, H.-P., Skobelev, I. Yu., Faenov, A. Ya., Soloviev, A., Huarte-Espinosa, M., Frank, A., Portugall, O., Pépin, H., Fuchs, J., École normale supérieure - Paris (ENS Paris), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut National des Sciences Appliquées - Toulouse (INSA Toulouse), and Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)

Subjects
jets, Physics, Jet (fluid), Multidisciplinary, Shock (fluid dynamics), Young stellar object, Astrophysics::High Energy Astrophysical Phenomena, Flow (psychology), Plasma, Conical surface, Astrophysics, 01 natural sciences, SIMULATIONS, 010305 fluids & plasmas, Magnetic field, COLLIMATION, [PHYS.COND.CM-S]Physics [physics]/Condensed Matter [cond-mat]/Superconductivity [cond-mat.supr-con], DISCOVERY, 0103 physical sciences, DG-TAURI, 010303 astronomy & astrophysics, ACCRETION DISCS, Astrophysics::Galaxy Astrophysics, DRIVEN JETS
Abstract

International audience; Although bipolar jets are seen emerging from a wide variety of astrophysical systems, the issue of their formation and morphology beyond their launching is still under study. Our scaled laboratory experiments, representative of young stellar object outflows, reveal that stable and narrow collimation of the entire flow can result from the presence of a poloidal magnetic field whose strength is consistent with observations. The laboratory plasma becomes focused with an interior cavity. This gives rise to a standing conical shock from which the jet emerges. Following simulations of the process at the full astrophysical scale, we conclude that it can also explain recently discovered x-ray emission features observed in low-density regions at the base of protostellar jets, such as the well-studied jet HH 154.

Published
2014
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4. Herschel/PACS observations of young sources in Taurus

Author

Göran Sandell, Giambattista Aresu, A. Mora, W. F. R. Dent, D. R. Flower, Christian D. Howard, Sean D. Brittain, Inga Kamp, Christophe Pinte, Linda Podio, Glenn J. White, and Astronomy

Subjects
010504 meteorology & atmospheric sciences, Young stellar object, Astrophysics::High Energy Astrophysical Phenomena, DRIVEN MOLECULAR OUTFLOW, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, HERBIG-HARO OBJECTS, 01 natural sciences, MASS-LOSS RATES, Far infrared, DARK CLOUD, 0103 physical sciences, ACCRETION RATES, Astrophysics::Solar and Stellar Astrophysics, DG-TAURI, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Line (formation), ISM: general, Physics, ADAPTIVE OPTICS, stars: formation, astrochemistry, Astronomy and Astrophysics, HUBBLE-SPACE-TELESCOPE, Accretion (astrophysics), ISM: molecules, ISM: jets and outflows, Orders of magnitude (time), Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, Excited state, Outflow, T-TAURI, Main sequence, DISK ACCRETION
Abstract

Observations of the atomic and molecular line emission associated with jets and outflows emitted by young stellar objects can be used to trace the various evolutionary stages they pass through as they evolve to become main sequence stars. To understand the relevance of atomic and molecular cooling in shocks, and how accretion and ejection efficiency evolves with the source evolutionary state, we will study the far-infrared counterparts of bright optical jets associated with Class I and II sources in Taurus (T Tau, DG Tau A, DG Tau B, FS Tau A+B, and RW Aur). We have analysed Herschel/PACS observations of a number of atomic ([OI]63um, 145um, [CII]158um) and molecular (high-J CO, H2O, OH) lines, collected within the OTKP GASPS. To constrain the origin of the detected lines we have compared the FIR emission maps with the emission from optical-jets and millimetre-outflows, and the line fluxes and ratios with predictions from shock and disk models. All of the targets are associated with extended emission in the atomic lines correlated with the direction of the optical jet/mm-outflow. The atomic lines can be excited in fast dissociative J-shocks. The molecular emission, on the contrary, originates from a compact region, that is spatially and spectrally unresolved. Slow C- or J- shocks with high pre-shock densities reproduce the observed H2O and high-J CO lines; however, the disk and/or UV-heated outflow cavities may contribute to the emission. While the cooling is dominated by CO and H2O lines in Class 0 sources, [OI] becomes an important coolant as the source evolves and the environment is cleared. The cooling and mass loss rates estimated for Class II and I sources are one to four orders of magnitude lower than for Class 0 sources. This provides strong evidence to indicate that the outflow activity decreases as the source evolves., 18 pages, 9 figures, accepted by A&A

Published
2012

5. Episodic Magnetic Bubbles and Jets: Astrophysical Implications from Laboratory Experiments

Author

Francisco Suzuki-Vidal, Adam Frank, Sergey Lebedev, Adam Harvey-Thompson, Eric G. Blackman, Max Camenzind, Andrea Ciardi, S. N. Bland, Gareth Hall, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Centre for Cold Matter, Blackett Laboratory, Imperial College London, Prince Consort Road, London SW7 2AZ, (CCM), Imperial College London, Department of Physics and Astronomy, University of Rochester, and Universität Heidelberg [Heidelberg] = Heidelberg University

Subjects
Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astronomy & Astrophysics, Collimated light, PHYSICS, FLOWS, Acceleration, Accretion disc, Protostar, Astrophysics::Solar and Stellar Astrophysics, ISM: Herbig-Haro objects, DG-TAURI, Magnetic bubbles, Astrophysics::Galaxy Astrophysics, Physics, Jet (fluid), Science & Technology, DISKS, Astrophysics (astro-ph), STABILITY PROPERTIES, Astronomy and Astrophysics, HUBBLE-SPACE-TELESCOPE, SIMULATIONS, EVOLUTION, XZ-TAURI, ISM: jets and outflows, Space and Planetary Science, Physical Sciences, Physics::Accelerator Physics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], ACCRETION DISCS
Abstract

Collimated outflows (jets) are ubiquitous in the universe appearing around sources as diverse as protostars and extragalactic supermassive blackholes. Jets are thought to be magnetically collimated, and launched from a magnetized accretion disk surrounding a compact gravitating object. We have developed the first laboratory experiments to address time-dependent, episodic phenomena relevant to the poorly understood jet acceleration and collimation region. The experimental results show the periodic ejections of magnetic bubbles naturally evolving into a heterogeneous jet propagating inside a channel made of self-collimated magnetic cavities. The results provide a unique view of the possible transition from a relatively steady-state jet launching to the observed highly structured outflows., Comment: 13 pages 4 Figures, revised version. Accepted for publication in the Astrophysical Journal Letters

Published
2008
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