Chemically active outflow L 1157

By R. Bachiller, M. P. Gutiérrez, M. Kumar, M. Tafalla. 2001

192 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Spectroscopy

View Paper: https://www.semanticscholar.org/paper/3b1fb2004cb0a489b63ddf62995cb017c89f9962

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. P. Myers
2. P. Caselli
3. M. Tafalla
4. Zhi-Yun Li
5. F. Nakamura
6. J. Jørgensen
7. T. Bourke
8. N. Evans II

In Spectroscopy

1. J. Jørgensen
2. M. Tafalla
3. E. V. van Dishoeck
4. P. Myers
5. F. Schoeier
6. T. Bourke
7. Zhi-Yun Li
8. F. Nakamura

Citations in the corpus

• A COLD COMPLEX CHEMISTRY TOWARD THE LOW-MASS PROTOSTAR B1-b: EVIDENCE FOR COMPLEX MOLECULE PRODUCTION IN ICES (2010, unknown): “Grain sputtering is often invoked to explain excess CH3OH in protostellar outflows (e.g. Bachiller et al. 2001) and is probably responsible for the factor of a few higher abundances of CH3OH gas in the two outflow positions around the dust core, using the same conversion factor as above to derive…”
• Protostellar Turbulence Driven by Collimated Outflows (2007, methodology): “…the bolometric luminosity Lbol comes from the accretion luminosity Lacc = GṀ∗M∗ R∗ (12) and that the mass accretion rate Ṁ∗ is given by M∗/tdyn, where M∗ is the stellar mass and tdyn is the dynamical time for the outflow, which is measured to be ∼ 3×10 4 years for L1157 (Bachiller et al. 2001).”
• PROSAC: A Submillimeter Array Survey of Low-Mass Protostars. I. Overview of Program: Envelopes, Disks, Outflows, and Hot Cores (2007, background): “L1157 MM L1157 MM is perhaps best known for its prominent outflow (Bachiller & Pérez Gutiérrez 1997; Bachiller et al. 2001), but also its small-scale envelope/disk structure has gotten a fair amount of attention.”
• Complex Molecules in the L1157 Molecular Outflow (2008, background): “…clearly demonstrated by multi-molecular line observations reflecting enhanced molecular abundances either in shocks associated with the outflows or in the outflow cavity walls in the protostellar envelopes (e.g., Garay et al. 1998; Bachiller et al. 2001; Arce & Sargent 2006; Jørgensen et al. 2007).”