Orion Nebula
No wide spread of stellar ages in the Orion Nebula Cluster
... The wide luminosity dispersion seen for stars at a given effective temperature in the Hertzsprung–Russell diagrams of young clusters and star-forming regions is often interpreted as due to significant (∼10 Myr) spreads ...
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Bootstrapping dielectronic recombination from second-row elements and the Orion Nebula
... Dielectronic recombination (DR) is the dominant recombination process for most heavy elements in photoionized clouds. Accurate DR rates for a species can be predicted when the positions of autoionizing states are known. ...
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A MUSE map of the central Orion Nebula (M 42)
... poorly flux-calibrated. They were shallow due to very short ex- posure time and of low spatial and spectral resolution. Some of these aspects (depth and spectral resolution) have been im- proved in a new mosaic mapping a ...
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Radio Measurements of the Stellar Proper Motions in the Core of the Orion Nebula Cluster
... Using multi-epoch Very Large Array observations, covering a time baseline of 29.1 years, we have measured the proper motions of 88 young stars with compact radio emission in the core of the Orion Nebula ...
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Spectroscopic Binaries in the Orion Nebula Cluster and NGC 2264
... The Orion Nebula Cloud ( ONC ) and NGC 2264 are two of the closest regions of clustered star formation ( d ∼ 400 pc and ∼ 900 pc, ages of 1 – 2 Myr and ...the Orion Molecular Clouds by Kounkel et ...
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Tearing the Veil: Interaction of the Orion Nebula with its Neutral Environment
... the Orion Nebula were carried out by Lockhart & Goss (1978) at an angular resolution of 2 , using the Owens Valley ...the Orion Nebula, first suggested by Lockhart & Goss (1978), based ...
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Is stellar multiplicity universal? Tight stellar binaries in the Orion nebula Cluster
... Estimating masses in the ONC population is a notoriously non- trivial issue because of crowding, confusion with the surrounding nebula and large and inhomogeneous line-of-sight extinction. As a result, while many ...
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Surveying young stars with Gaia: Orion and the Solar neighbourhood
... The age map of Fig. 4.9 suggests that multiple star formation episodes can oc- cur within the same region and give limits on the duration of a single star formation episode. We notice that a global trend between the ...
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Nested Shells Reveal the Rejuvenation of the Orion-Eridanus Superbubble
... the Orion – Eridanus region must have been highly episodic over the past 10 – 15 ...the Orion – Eridanus superbubble consists of a set of nested ...the Orion – Eridanus superbubble, such as the ...
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Hops 383: an Outbursting Class 0 Protostar in Orion
... have extended the outburst phenomenon to the envelope- embedded Class I protostars. Such protostellar outbursts include V346 Nor ( Graham & Frogel 1985 ) , OO Ser ( Hodapp et al. 1996; Kóspál et al. 2007 ) , V1647 ...
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NGC 1980 is not a foreground population of Orion : spectroscopic survey of young stars with low extinction in Orion A
... band and Spitzer 8 µm band can be 0.5 less than the observed spectral slopes. In Fig. 20, we compare the me- dian SED of class II sources in this work with those in Orion nebula cluster (ONC, 1 Myr), L1641 ...
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Ultra-high-resolution spectroscopy of the ISM towards Orion
... Model fits have been constructed for the absorption-line profiles, providing estim ates for the column density, velocity dispersion, and central velocity for each constituent veloc ity component. These d a ta enable the ...
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Orion revisited : III The Orion Belt population
... the Orion A cloud but seen in projection toward ...larger Orion star formation complex and not in the existing Orion A molecular cloud like, for example, the Orion nebula ...the ...
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Three-dimensional magnetohydrodynamic simulations of the Crab Nebula
... the nebula, whereas in our model we followed Kennel & Coroniti (1984b) and assumed that they are accelerated only at the termination ...the nebula (not ...outer nebula, both the polarization and ...
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The demographics of protoplanetary disks: from Lupus to Orion
... Working in science is a privilege to begin with; but I feel very grateful at how welcoming, friendly, and open I have found this community. That is true in general, and in particular for the many people who have been ...
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Physical conditions in the planetary nebula Abell 30
... The extremely low temperatures measured from oxygen recombi- nation lines, together with the extremely high heavy element abun- dances relative to hydrogen, show that the two polar knots J1 and J3 analysed here must ...
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Thermal evolution of icy planetesimals in the solar nebula
... In this paper, a thermal evolution model of icy planetesi- mals is constructed, and the temperature evolutions are nu- merically solved with various values of parameters (size, initial abundance of 26 Al and initial ...
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Discovering Planetary Nebula Geometries: Explorations with a Hierarchy of Models
... Our basic approach utilizes a hierarchy of models of increasing complexity. Earlier studies establish that a hierarchical sequence converges more quickly, and to a better solution, than a search relying only on the most ...
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Rayleigh-Taylor instability in magnetohydrodynamic simulations of the Crab nebula
... Crab nebula. These features can be as long as the nebula radius and they do not appear to be stream- ing radially towards its centre (see ...Crab nebula and these filaments designate ‘valleys’, where ...
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The blue supergiant MN18 and its bipolar circumstellar nebula
... the nebula (Sonneborn et ...bipolar nebula around this star, which in turn would help to better understand the origin of bipolar nebulae around other massive ...
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