The Nature and Frequency of Outflows from Stars in the Central Orion Nebula Cluster
arXiv:1508.03412 · doi:10.1088/0004-6256/150/4/108
Abstract
Recent Hubble Space Telescope images have allowed the determination with unprecedented accuracy of motions and changes of shocks within the inner Orion Nebula. These originate from collimated outflows from very young stars, some within the ionized portion of the nebula and others within the host molecular cloud. We have doubled the number of Herbig-Haro objects known within the inner Orion Nebula. We find that the best-known Herbig-Haro shocks originate from a relatively few stars, with the optically visible X-ray source COUP 666 driving many of them. While some isolated shocks are driven by single collimated outflows, many groups of shocks are the result of a single stellar source having jets oriented in multiple directions at similar times. This explains the feature that shocks aligned in opposite directions in the plane of the sky are usually blue shifted because the redshifted outflows pass into the optically thick Photon Dominated Region behind the nebula. There are two regions from which optical outflows originate for which there are no candidate sources in the SIMBAD data base.
152 pages, 46 figures, 7 tables. Accepted by AJ
References in corpus (12)
- Million-Degree Plasma Pervading the Extended Orion Nebula
- Tracing the young massive high-eccentricity binary system Theta 1 Orionis C through periastron passage
- Properties of the ionized gas in HH202. II: Results from echelle spectrophotometry with UVES
- X-ray properties of protostars in the Orion Nebula
- The three dimensional dynamic structure of the inner Orion Nebula
- A Multi-Color Optical Survey of the Orion Nebula Cluster. Part I: the Catalog
- Silicon Monoxide Observations Reveal a Cluster of Hidden Compact Outflows in the OMC1 South Region
- High Velocity Features in the Orion Nebula
- Large Scale Flows from Orion-South
- NICMOS Observations of Shocked H_2 in Orion
- ALMA Observations of the Largest Proto-Planetary Disk in the Orion Nebula, 114-426: A CO Silhouette
- A photoionized Herbig-Haro object in the Orion nebula
Cited by in corpus (20)
- Understanding Galaxy Evolution through Emission Lines
- Nebular spectroscopy: A guide on H II regions and planetary nebulae
- The ALMA View of the OMC1 Explosion in Orion
- PDRs4All II: JWST's NIR and MIR imaging view of the Orion Nebula
- Turbulence in the Ionized Gas of the Orion Nebula
- Photoionized Herbig-Haro objects in the Orion Nebula through deep high-spectral resolution spectroscopy I: HH529II and III
- Structure and Physical Conditions in the Huygens Region of the Orion Nebula
- Small Protoplanetary Disks in the Orion Nebula Cluster and OMC1 with ALMA
- Cradle(s) of the Sun
- Photoionized Herbig-Haro objects in the Orion Nebula through deep high-spectral resolution spectroscopy II: HH204
- Photoionized Herbig-Haro objects in the Orion Nebula through deep high-spectral resolution spectroscopy III: HH514
- Messenger Monte-Carlo MAPPINGS V (M^3) -- A self-consistent three-dimensional photoionization code
- Layers in the Central Orion Nebula
- Dents in the Veil: Protostellar feedback in Orion
- A Molecular Line Survey around Orion at Low Frequencies with the MWA
- Deciphering the 3-D Orion Nebula-III: Structure on the NE boundary of the Orion-S Embedded Molecular Cloud
- SDSS-V LVM: Resolving Physical Conditions in the Trifid Nebula
- Low-Frequency Carbon Recombination Lines in the Orion Molecular Cloud Complex
- Large Scale Wind Driven Structures in the Orion Nebula
- Deciphering the 3-D Orion Nebula-IV: The HH~269 flow emerges from the Orion-S Embedded Molecular Cloud