Astronomy and Astrophysics – Astronomy
Scientific paper
Oct 2004
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004apj...614l..69h&link_type=abstract
The Astrophysical Journal, Volume 614, Issue 1, pp. L69-L71.
Astronomy and Astrophysics
Astronomy
15
Ism: Herbig-Haro Objects, Ism: Jets And Outflows, Shock Waves
Scientific paper
We predict fluxes for the brightest lines of [Fe II] at wavelengths longer than 8000 Å for several radiative shocks whose parameters resemble those typically present in stellar jets. The models show that the brightest lines are those at 1.257, 1.643, 5.340, 17.94, and 25.99 μm. Depending on the model, these lines typically have comparable fluxes and are usually brighter than the [O I] 63.3 μm and [Si II] 34.8 μm lines. We call attention to the 5.34 μm line of Fe II, which cannot be seen from the ground but should be easily observable with the Spitzer satellite and SOFIA for many sources. This line should be an excellent probe of outflows from the youngest stars; at mid-IR wavelengths, it penetrates through most dusty regions of star formation, yet has a short enough wavelength to retain good spatial resolution in diffraction-limited images obtainable from space.
Hartigan Patrick
Pierson Rachel
Raymond John
No associations
LandOfFree
Infrared Emission Lines of [Fe II] as Diagnostics of Shocked Gas in Stellar Jets does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Infrared Emission Lines of [Fe II] as Diagnostics of Shocked Gas in Stellar Jets, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Infrared Emission Lines of [Fe II] as Diagnostics of Shocked Gas in Stellar Jets will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-898093