2018
DOI: 10.1007/s00159-018-0107-z
|View full text |Cite
|
Sign up to set email alerts
|

Radio jets from young stellar objects

Abstract: Jets and outflows are ubiquitous in the process of formation of stars since outflow is intimately associated with accretion. Free-free (thermal) radio continuum emission in the centimeter domain is associated with these jets. The emission is relatively weak and compact, and sensitive radio interferometers of high angular resolution are required to detect and study it. One of the key problems in the study of outflows is to determine how they are accelerated and collimated. Observations in the cm range are most … Show more

Help me understand this report
View preprint versions

Search citation statements

Order By: Relevance

Paper Sections

Select...
1
1
1
1

Citation Types

24
149
2

Year Published

2019
2019
2023
2023

Publication Types

Select...
7
2
1

Relationship

1
9

Authors

Journals

citations
Cited by 130 publications
(175 citation statements)
references
References 323 publications
(256 reference statements)
24
149
2
Order By: Relevance
“…The result of the above equation is given in units of 10 -6 M ⊙ year -1 . We adopted θ = 10° since the usually high collimation of jets allow for a small opening angle, v = 200 km s -1 as typical jet velocity for low-mass objects, the inclination, i, determined from the source sizes (see main text) and T = 10 4 K is usually adopted (29). Despite the flux calibration uncertainties at centimetric-wavelength observations being normally lower than millimetric ones, we assume a conservative uncertainty for the VLA fluxes to be similar to the ALMA data, 15%.…”
Section: Ionized Mass Loss Rate From Each Protobinary Componentmentioning
confidence: 99%
“…The result of the above equation is given in units of 10 -6 M ⊙ year -1 . We adopted θ = 10° since the usually high collimation of jets allow for a small opening angle, v = 200 km s -1 as typical jet velocity for low-mass objects, the inclination, i, determined from the source sizes (see main text) and T = 10 4 K is usually adopted (29). Despite the flux calibration uncertainties at centimetric-wavelength observations being normally lower than millimetric ones, we assume a conservative uncertainty for the VLA fluxes to be similar to the ALMA data, 15%.…”
Section: Ionized Mass Loss Rate From Each Protobinary Componentmentioning
confidence: 99%
“…radiation with a positive spectral index α where the flux at frequency ν, S ν ∝ ν α ). Moreover, typical flux densities are very low and usually less than 1 mJy [Anglada et al, 2018]. Such emission is un-polarized and is often elongated in the direction of the known atomic/molecular outflow.…”
Section: What Radio Emission From Outflows Can Tell Usmentioning
confidence: 99%
“…For example, no clear outflow has been detected from HOPS-108 itself in 12 CO molecular line emission, and the free-free continuum source associated with HOPS-108 is very weak in comparison with HOPS-370. There is a known correlation between L bol and free-free continuum emission (Anglada 1995;Shirley et al 2007;Tychoniec et al 2018;Anglada et al 2018). If HOPS-108 is consistent with the correlation derived by Tychoniec et al (2018), then a 100 L source is expected to have a 4.1 cm flux density of ∼1.5 mJy at the distance to Orion.…”
Section: Remaining Questionsmentioning
confidence: 99%