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Artykuły w czasopismach na temat "Protostellar jets"
Hayashi, Mitsuru, Kazunari Shibata i Ryoji Matsumoto. "Flares and MHD Jets in Protostar". Symposium - International Astronomical Union 188 (1998): 232–33. http://dx.doi.org/10.1017/s0074180900114901.
Pełny tekst źródłaVorobyov, Eduard I., Vardan G. Elbakyan, Adele L. Plunkett, Michael M. Dunham, Marc Audard, Manuel Guedel i Odysseas Dionatos. "Knotty protostellar jets as a signature of episodic protostellar accretion?" Astronomy & Astrophysics 613 (maj 2018): A18. http://dx.doi.org/10.1051/0004-6361/201732253.
Pełny tekst źródłaReipurth, Bo, Luis F. Rodrguez, Guillem Anglada i John Bally. "Radio Continuum Jets from Protostellar Objects". Astronomical Journal 127, nr 3 (marzec 2004): 1736–46. http://dx.doi.org/10.1086/381062.
Pełny tekst źródłaStone, James M., i Philip E. Hardee. "Magnetohydrodynamic Models of Axisymmetric Protostellar Jets". Astrophysical Journal 540, nr 1 (wrzesień 2000): 192–210. http://dx.doi.org/10.1086/309289.
Pełny tekst źródłade Gouveia dal Pino, Elisabete M., i Willy Benz. "Three-dimensional simulations of protostellar jets". Astrophysical Journal 410 (czerwiec 1993): 686. http://dx.doi.org/10.1086/172785.
Pełny tekst źródłaReipurth, Bo, John Bally, Robert A. Fesen i David Devine. "Protostellar jets irradiated by massive stars". Nature 396, nr 6709 (listopad 1998): 343–45. http://dx.doi.org/10.1038/24562.
Pełny tekst źródłaZinnecker, Hans, i Mark J. McCaughrean. "Infrared Jets from Protostars: The case of HH212". International Astronomical Union Colloquium 163 (1997): 531–35. http://dx.doi.org/10.1017/s0252921100043153.
Pełny tekst źródłaSpruit, H. C. "Jets from Compact Objects". Symposium - International Astronomical Union 195 (2000): 113–22. http://dx.doi.org/10.1017/s0074180900162849.
Pełny tekst źródłaShibata, Kazunari. "Theory of Flares and MHD Jets". Symposium - International Astronomical Union 188 (1998): 9–12. http://dx.doi.org/10.1017/s0074180900114317.
Pełny tekst źródłaPodio, Linda, Benoit Tabone i 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.
Pełny tekst źródłaRozprawy doktorskie na temat "Protostellar jets"
Čemeljić, Miljenko. "Resistive magnetohydrodynamic jets from protostellar accretion disks". [S.l. : s.n.], 2004. http://deposit.ddb.de/cgi-bin/dokserv?idn=974114529.
Pełny tekst źródłaCemeljic, Miljenko. "Resistive magnetohydrodynamic jets from protostellar accretion disks". Phd thesis, Universität Potsdam, 2005. http://opus.kobv.de/ubp/volltexte/2005/209/.
Pełny tekst źródłaIn this thesis the magnetohydrodynamic jet formation and the effects of magnetic diffusion on the formation of axisymmetric protostellar jets have been investigated in three different simulation sets. The time-dependent numerical simulations have been performed, using the magnetohydrodynamic ZEUS-3D code.
Waugh, Jonathan Nicholas. "Modelling of protostellar jets using intense lasers". Thesis, University of York, 2010. http://etheses.whiterose.ac.uk/1468/.
Pełny tekst źródłaRabenanahary, Mialy Rabetanety. "Flots protostellaires poussés par un jet dans une enveloppe stratifiée : revisiter un modèle à l'ère d'ALMA". Electronic Thesis or Diss., Université Paris sciences et lettres, 2022. http://www.theses.fr/2022UPSLO014.
Pełny tekst źródłaA long-standing open question in star formation is the process responsible for its low efficiency on parsec scales (a few %), and for shifting down the Initial Mass Function (IMF) to only ∼30% of the prestellar core mass distribution. The most recent numerical simulations show that neither turbulence nor magnetic fields can, alone, reproduce these low efficiencies, and that feedback by protostellar outflows must play a crucial role by disrupting accretion streams, expelling material from cores, and/or sustaining turbulence. Unfortunately, the magnitude of outflow feedback (affected cloud volume, injected momentum, entrained mass, impact on the disk and infalling envelope) depends strongly on the underlying protostellar wind geometry, which remains uncertain and heavily debated: a fast wide-angle "X-wind”, a slower MHD disk wind, a narrow jet ? Clearly, if we want to reliably assess the role of outflow feedback in star formation, it is of utmost importance to determine which wind geometry is the most realistic (and/or which one can be excluded). As a new contribution towards this goal, we present, for the first time, numerical predictions for outflows driven by a narrow pulsed jet in a stratified prestellar core. We compare our simulations against recent ALMA observations and analogous predictions for a wide-angle X-wind. Our simulations are the first to combine jet variability, ambient density-stratification, and long timescales up to 10 000 yrs (typical of young outflows) on scales up to 0.1 pc. We find that the predicted widths, position-velocity diagrams, and mass-velocity distribution, show striking resemblance with ALMA observations of CO outflows such as HH46/47 and CARMA-7, and in closer agreement than models based on a wide-angle "X-wind". The results obtained in this work could have major implications for the feedback of protostellar outflows on star formation
GARCIA, LOPEZ REBECA. "Near infrared diagnostics of Class 0/I protostars: the jets and accretion region". Doctoral thesis, Università degli Studi di Roma "Tor Vergata", 2009. http://hdl.handle.net/2108/815.
Pełny tekst źródłaIn this thesis a study of the accretion and ejection properties of low mass embedded protostar (the so-called Class 0/I sources) through ISAAC NIR high angular observations is presented. The physics, kinematics and dynamics of five Class 0/I jets (HH1, HH111,HH212 / HH34, HH46-47) have been analysed in order to give some insights about the jet generation and the dependence of the jet properties on the evolutionary stage of the source. In addition, the accretion properties of a sample of ten Class I sources have been measured in order to revise their evolutionary status. All the studied jets have been observed through atomic and molecular emission, traced by [FeII] and H2 transitions. Applying near-IR diagnostic techniques important physical parameters have been inferred. In particular, one milestone of this thesis was to derive the physical properties of embedded protostellar jets as a function of the jet radial velocity. For instance, at large distances from the source, the electron density (ne) has been found to decrease with lower velocities. Average values over the brightest knots of 2600-6200 cm3 have been found. The amount of mass transported along the flows has been also inferred. The results show that Class 0/I jets transport more mass than the more evolved jets from CTTS, while the accretion to ejection ratio remains roughly constant independently of the evolutionary stage of the source. The inner region of Class I jets has been studied in detail in order to constrain the jet launching mechanism. Similarly to what found in CTTS jets, Class I jets present two velocity components at high and low velocity (the HVC and LVC) in both the atomic and molecular gas. The LVC in Class I jets reaches, however, larger distances (up to 1000 AU from the source) with respect to jets from CTTS. At variance with what found at large distances from the source, in the inner jet region, ne increases with decreasing velocity, while the mass flux along the jet is always higher in the HVC. When comparing these results with the predictions of MHD jet launching models, the kinematical characteristics of the line emission are found to be, at least qualitatively, reproduced by the studied models. None of them can explain, however, the extent of the LVC and the velocity dependence of electron density that is observed. On the other hand, the study of the set of Class I sources reveals no clear correlation between accretion and ejection features. In addition, in spite of what is expected by embedded protostars, only four of the ten sources show accretion dominated luminosities. This result suggests that most of the objects considered as Class I sources are, instead, more evolved sources that have already acquired most of their mass. Despite this fact, the inferred mass accretion rates are larger that those found in CTTS of the same mass.
Stanke, Thomas. "An unbiased infrared H2 search for embedded flows from young stars in Orion A". Phd thesis, Universität Potsdam, 2000. http://opus.kobv.de/ubp/volltexte/2005/20/.
Pełny tekst źródłaDas erste Ergebnis ist, dass Ausströmungen in Sternentstehungsgebieten tatsächlich sehr häufig sind: mehr als 70 Jet-Kandidaten werden identifiziert. Die meisten zeigen eine sehr irreguläre Morphologie anstelle regulärer oder symmetrischer Strukturen. Dies ist auf das turbulente, klumpige Medium zurückzuführen, in das sich die Jets hineinbewegen. Die Ausrichtung der Jets ist zufällig verteilt. Insbesondere gibt es keine bevorzugte Ausrichtung der Jets parallel zum grossräumigen Magnetfeld in der Wolke. Das legt nahe, dass die Rotations- und Symmetrieachse in einem protostellaren System durch zufällige, turbulente Bewegung in der Wolke bestimmt wird.
Mögliche Ausströmungsquellen werden für 49 Jets identifiziert; für diese wird der Entwicklungsstand und die bolometrische Leuchtkraft abgeschätzt. Die Jetlänge und die H2 Leuchtkraft entwickeln sich gemeinsam mit der Ausströmungsquelle. Von null startend, dehnen sich die Jets schnell bis auf eine Länge von einigen Parsec aus und werden dann langsam wieder kürzer. Sie sind zuerst sehr leuchtkräftig, die H2 Helligkeit nimmt aber im Lauf der protostellaren Entwicklung ab. Die Längen- und H2 Leuchtkraftentwicklung lässt sich im Wesentlichen durch eine zuerst sehr hohe, dann niedriger werdende Massenausflussrate erklären, die auf eine zuerst sehr hohe, dann niedriger werdende Gasakkretionsrate auf den Protostern schliessen lässt (Akkretion und Ejektion sind eng verknüpft!). Die Längenabnahme der Jets erfordert eine ständig wirkende Abbremsung der Jets. Ein einfaches Modell einer simultanen Entwicklung eines Protosterns, seiner zirkumstellaren Umgebung und seiner Ausströmung (Smith 2000) kann die gemessenen H2- und bolometrischen Leuchtkräfte der Jets und ihrer Quellen reproduzieren, unter der Annahme, dass die starke Akkretionsaktivität zu Beginn der protostellaren Entwicklung mit einer überproportional hohen Massenausflussrate verbunden ist.
Im Durchmusterungsgebiet sind 125 dichte Molekülwolkenkerne bekannt (Tatematsu et al. 1993). Jets (bzw. Sterne) entstehen in ruhigen Wolkenkernen, d.h. solchen mit einem niedrigen Verhältnis von interner kinetischer Energie zu gravitativer potentieller Energie; dies sind die Wolkenkerne höherer Masse. Die Wolkenkerne mit Jets haben im Mittel grössere Linienbreiten als die ohne Jets. Dies ist darauf zurückzuführen, dass sie bevorzugt in den massereicheren Wolkenkernen zu finden sind, welche generell eine grössere Linienbreite haben. Es gibt keinen Hinweis auf stärkere interne Bewegungen in Wolkenkernen mit Jets, die durch eine Wechselwirkung der Jets mit den Wolkenkernen erzeugt sein könnte. Es gibt, wie von der Theorie vorausgesagt, eine Beziehung zwischen der Linienbreite der Wolkenkerne und der H2 Leuchtkraft der Jets, wenn Jets von Klasse 0 und Klasse I Protosternen separat betrachtet werden; dabei sind Klasse 0 Jets leuchtkräftiger als Klasse I Jets, was ebenfalls auf eine zeitabhängige Akkretionsrate mit einer frühzeitigen Spitze und einem darauffolgenden Abklingen hinweist.
Schliesslich wird die Rückwirkung der Jetpopulation auf eine Molekülwolke unter der Annahme strikter Vorwärtsimpulserhaltung betrachtet. Die Jets können auf der Skala einer ganzen Riesenmolekülwolke und auf den Skalen von Molekülwolkenkernen nicht genügend Impuls liefern, um die abklingende Turbulenz wieder anzuregen. Auf der mittleren Skala von molekularen Klumpen, mit einer Grösse von einigen parsec und Massen von einigen hundert Sonnenmassen liefern die Jets jedoch genügend Impuls in hinreichend kurzer Zeit, um die Turbulenz “am Leben zu erhalten” und können damit helfen, einen Klumpen gegen seinen Kollaps zu stabilisieren.
The presence of outflows, often in the form of well-collimated jets, is a phenomenon commonly associated with the birth of young stars. Emission from shock-excited molecular hydrogen at near-infrared wavelengths is one of the signposts of the presence of such an outflow, and generally can be observed even if the flow is obscured at optical wavelengths. In this thesis, I present the results of an unbiased, sensitive, wide-field search for flows from protostellar objects in the H2 v=1-0 S(1) line at a wavelength of 2.12 µm, covering a 1 square degree area of the Orion A giant molecular cloud. Further data covering a wide wavelength range are used to search for the driving sources of the flows. The aim of this work is to obtain a sample of outflows which is free from biases as far as possible, to derive the typical properties of the outflows, to search for evolutionary trends, and to examine the impact of outflows on the ambient cloud.
The first result from this survey is that outflows are indeed common in star forming regions: more than 70 candidate jets are identified. Most of them have a fairly ill-defined morphology rather than a regular or symmetric structure, which is interpreted to be due to the turbulent, clumpy ambient medium into which the jets are propagating. The jets are randomly oriented. In particular, no alignment of the jets with the large scale ambient magnetic field is found, suggesting that the spin and symmetry axis in a protostellar object is determined by random, turbulent motions in the cloud.
Candidate driving sources are identified for 49 jets, and their evolutionary stage and bolometric luminosity is estimated. The jet lengths and H2 luminosities evolve as a function of the age of the driving source: the jets grow quickly from zero length to a size of a few parsec and then slowly shorten again. The jets are very luminous early on and fade during the protostellar evolution. The evolution in length and H2 luminosity is attributed to an early phase of strong accretion, which subsequently decreases. The shortening of the jets with time requires the presence of a continuous deceleration of the jets. A simple model of the simultaneous evolution of a protostar, its circumstellar environment, and its outflow (Smith 2000) can reproduce the measured values of H2 luminosity and driving source luminosity under the assumption of a strong accretion plus high ejection efficiency phase early in the protostellar evolution.
Tatematsu et al. (1993) found 125 dense cloud cores in the survey area. The jet driving sources are found to have formed predominantly in quiet cores with a low ratio of internal kinetic energy to gravitational potential energy; these are the cores with higher masses. The cores which are associated with jets have on average larger linewidths than cores without jets. This is due to the preferred presence of jets in more massive cores, which generally have larger linewidths. There is no evidence for additional internal motions excited by the interaction of the jets with the cores. The jet H2 luminosity and the core linewidth (as predicted by theory) are related, if Class 0 and Class I jets are considered separately; the relation lies at higher values of the H2 luminosity for the Class 0 jets than for Class I jets. This also suggests a time evolution of the accretion rate, with a strong peak early on and a subsequent decay.
Finally, the impact of a protostellar jet population on a molecular cloud is considered. Under the conservative assumption of strict forward momentum conservation, the jets appear to fail to provide sufficient momentum to replenish decaying turbulence on the scales of a giant molecular cloud and on the scales of molecular cloud cores. At the intermediate scales of molecular clumps with sizes of a few parsec and masses of a few hundred solar masses, the jets provide enough momentum in a short enough time to potentially replenish turbulence and thus might help to stabilize the clump against further collapse.
Verliat, Antoine. "Origine du moment cinétique et influence des jets protostellaires sur la formation d'étoiles". Electronic Thesis or Diss., université Paris-Saclay, 2021. http://www.theses.fr/2021UPASP058.
Pełny tekst źródłaThe interstellar medium is the cradle of stars. It is a fantastic playground for physicists due to its richness and the complexity of the phenomena involved. Understanding the details of star formation is one of the great challenges of modern astrophysics.The complexity of the problems studied in this thesis makes numerical simulations a valuable tool. It has allowed me to study two fundamental aspects of star formation. The first part of my work is devoted to understanding the origin of the rotation of the disks made of gas and dust that surround young stars and in which planets form. The second is the study of the formation of star clusters. While it is known that stars form in clusters, the processes that influence the formation of these clusters and their structure are poorly understood. The study will focus particularly on the influence of jets of matter emitted by young stars on these clusters
Čemeljić, Miljenko [Verfasser]. "Resistive magnetohydrodynamic jets from protostellar accretion disks / von Miljenko Čemeljić". 2004. http://d-nb.info/974114529/34.
Pełny tekst źródłaO'Sullivan, Jamie [Verfasser]. "Molecular cooling and emissions in large scale simulations of protostellar jets / put forward by Jamie O'Sullivan". 2009. http://d-nb.info/999384325/34.
Pełny tekst źródłaNolan, Christopher. "Understanding Protostellar Jet Feedback on Disc and Cloud Scales". Phd thesis, 2019. http://hdl.handle.net/1885/195683.
Pełny tekst źródłaKsiążki na temat "Protostellar jets"
Tsinganos, Kanaris, Tom Ray i Matthias Stute, red. Protostellar Jets in Context. Berlin, Heidelberg: Springer Berlin Heidelberg, 2009. http://dx.doi.org/10.1007/978-3-642-00576-3.
Pełny tekst źródłaProtostellar jets in context. Berlin: Springer, 2009.
Znajdź pełny tekst źródłaTom Ray,Kanaris Tsinganos,Matthias Stute. Protostellar Jets in Context. Springer, 2009.
Znajdź pełny tekst źródłaRay, Tom, Kanaris Tsinganos i Matthias Stute. Protostellar Jets in Context. Springer London, Limited, 2009.
Znajdź pełny tekst źródłaRay, Tom, Kanaris Tsinganos i Matthias Stute. Protostellar Jets in Context. Springer, 2012.
Znajdź pełny tekst źródłaCzęści książek na temat "Protostellar jets"
Turner, Neal, Michal Różyczka i Peter Bodenheimer. "Driving Protostellar Jets". W Numerical Astrophysics, 183–84. Dordrecht: Springer Netherlands, 1999. http://dx.doi.org/10.1007/978-94-011-4780-4_59.
Pełny tekst źródłaLivio, Mario. "Astrophysical Jets". W Protostellar Jets in Context, 3–9. Berlin, Heidelberg: Springer Berlin Heidelberg, 2009. http://dx.doi.org/10.1007/978-3-642-00576-3_1.
Pełny tekst źródłaCoffey, Deirdre, Francesca Bacciotti, Antonio Chrysostomou, Brunetta Nisini i Chris Davis. "Searching for Jet Rotation Signatures in Class 0 and I Jets". W Protostellar Jets in Context, 241–45. Berlin, Heidelberg: Springer Berlin Heidelberg, 2009. http://dx.doi.org/10.1007/978-3-642-00576-3_29.
Pełny tekst źródłaBally, John. "Jets from Young Stars". W Protostellar Jets in Context, 11–20. Berlin, Heidelberg: Springer Berlin Heidelberg, 2009. http://dx.doi.org/10.1007/978-3-642-00576-3_2.
Pełny tekst źródłaNisini, Brunella. "Jets from Embedded Protostars". W Protostellar Jets in Context, 215–24. Berlin, Heidelberg: Springer Berlin Heidelberg, 2009. http://dx.doi.org/10.1007/978-3-642-00576-3_26.
Pełny tekst źródłaKryvdyk, Volodymyr. "Jets from Collapsing Stars". W Protostellar Jets in Context, 559–61. Berlin, Heidelberg: Springer Berlin Heidelberg, 2009. http://dx.doi.org/10.1007/978-3-642-00576-3_76.
Pełny tekst źródłaCai, Kai, Jan Staff, Brian P. Niebergal, Ralph E. Pudritz i Rachid Ouyed. "Large-scale 3D Simulations of Protostellar Jets: Long-term Stability and Jet Rotation". W Protostellar Jets in Context, 551–53. Berlin, Heidelberg: Springer Berlin Heidelberg, 2009. http://dx.doi.org/10.1007/978-3-642-00576-3_74.
Pełny tekst źródłaVlahakis, Nektarios. "Jets in the MHD Context". W Protostellar Jets in Context, 205–11. Berlin, Heidelberg: Springer Berlin Heidelberg, 2009. http://dx.doi.org/10.1007/978-3-642-00576-3_25.
Pełny tekst źródłaRaga, Alejandro C., Jorge Cantó, Fabio De Colle, Alejandro Esquivel, Primoz Kajdic, Ary Rodríguez- González i Pablo F. Velázquez. "Radiative Jets from Variable Sources". W Protostellar Jets in Context, 295–303. Berlin, Heidelberg: Springer Berlin Heidelberg, 2009. http://dx.doi.org/10.1007/978-3-642-00576-3_35.
Pełny tekst źródłaAkashi, Muhammad. "Shaping Planetary Nebulae by Jets". W Protostellar Jets in Context, 507–10. Berlin, Heidelberg: Springer Berlin Heidelberg, 2009. http://dx.doi.org/10.1007/978-3-642-00576-3_63.
Pełny tekst źródłaStreszczenia konferencji na temat "Protostellar jets"
de Gouveia Dal Pino, Elisabete M. "Protostellar jets: The best laboratories to investigate astrophysical jets". W International conference on plasma physics ICPP 1994. AIP, 1995. http://dx.doi.org/10.1063/1.49003.
Pełny tekst źródłaAraudo, Anabella, Marco Padovani i Alexandre Marcowith. "Cosmic ray acceleration and gamma-ray emission from protostellar jets". W 37th International Cosmic Ray Conference. Trieste, Italy: Sissa Medialab, 2021. http://dx.doi.org/10.22323/1.395.0684.
Pełny tekst źródłaLorenzetti, Dario, Teresa Giannini, Brunella Nisini, Fabrizio Vitali i Alessio Caratti o Garatti. "VLT-ISAAC spectroscopy of H 2 pure rotational lines: a new tool for investigating protostellar jets". W Astronomical Telescopes and Instrumentation, redaktor Puragra Guhathakurta. SPIE, 2003. http://dx.doi.org/10.1117/12.456512.
Pełny tekst źródłaBonito, R., C. V. M. Fridlund, F. Favata, G. Micela, G. Peres, A. A. Djupvik, R. Liseau i Eric Stempels. "The nearest X-ray emitting protostellar jet observed with HST". W COOL STARS, STELLAR SYSTEMS AND THE SUN: Proceedings of the 15th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun. AIP, 2009. http://dx.doi.org/10.1063/1.3099117.
Pełny tekst źródłaMotogi, Kazuhito, Kazuo Sorai, Kenta Fujisawa, Koichiro Sugiyama, Kotaro Niinuma i Mareki Honma. "The remarkable blue-shift dominated jet in the high mass protostellar object G353.273+0.641". W 11th European VLBI Network Symposium & Users Meeting. Trieste, Italy: Sissa Medialab, 2016. http://dx.doi.org/10.22323/1.178.0033.
Pełny tekst źródłaGoddi, Ciriaco, Gabriele Surcis i Luca Moscadelli. "Measuring Magnetic Fields from Water Masers Associated with the Synchrotron Protostellar Jet in W3(H2O)". W 14th European VLBI Network Symposium & Users Meeting. Trieste, Italy: Sissa Medialab, 2019. http://dx.doi.org/10.22323/1.344.0039.
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