protostellar jets and outflows — what alma can achieve? — 平野 尚美 (naomi hirano)...
TRANSCRIPT
Protostellar jets and outflows — what ALMA can achieve? —
平野 尚美 (Naomi Hirano)中研院天文所 (ASIAA)
Back to 1980... Discovery of the bipolar molecular
outflow from L1551 IRS5
Snell, Loren & Plambeck (1980)
A scenario of star formation
Why we study jets and outflows?
Jets are ubiquitous
from proto brown dwarfs (possibly proto planets), protostars, evolved stars, to active galactic nuclei
Key words
accretion, angular momentum, bipolar
Jets from young stellar objects (protostars)
spectroscopic observations allow us to study their kinematics → driving mechanism
Issues to be addressed‣ Can we see the primary jet ejected from the star?
CO outflows are likely to be swept-up ambient gas ≠
primary ejecta
‣ Are the jets and outflows transferring the excess
angular momentum from accreting material?
‣ Roles of magnetic field
Flow geometry v.s. magnetic field
‣ When and how jets and outflows start, and how they
evolve?
Highly-collimated jet from HH211
driving source:
cold (Tbol ~ 33 K) and low
luminosity (3.6 Lsun) protostar
CO J=2-1 observed with the JCMT
angular resolution: 20”
McCaughrean et al. (1994)Low velocity
- a pair of cavities
High velocity- narrow jet
CO J=2-1 observed with the PdBI
angular resolution: 1.5”
Gueth et al. (1999)
Highly-collimated jet:an important link between the primary jet and entrained outflow
HH211
Green: H2 in NIR, Blue & Red: SiO J=5-4Hirano et al. (2006)
Current achievement with the SMA
HH211SiO J=8-7
0.46”x 0.36”
0.35”x 0.23”
0.24”x 0.22”
Lee et al. (2009)
The innermost pair of knots
‣C-shaped bending
‣~4 sub-knots
‣transverse width < 40 AU
Observations with ALMA — 1
Search for the evidence of jet
rotation
Launhardt et al. (2009)
‣ Theoretical prediction
The jet is carrying out the excess angular momentum from accreting material
➡ The jet is spinning?
‣ Observationally, only one clear example has been known
‣ CO J=2-1 jet in CB26
• 1 Myr old star
• much older than the protostars in main accretion phase (< 105 yr)
The velocity gradient across the SiO jet in HH211
— a hint of jet rotation? —
- The NE side of the jet shows slightly larger velocity as compared to the SW side
- The mean velocity gradient
~0.5 km/s at ~10 AU (0.035”)
0.24” x 0.22”0.1” x 0.1”
Lee et al. (2009)
The velocity gradient across the SiO jet in HH212
SN: ~1 km/s @ 24 AUSS: ~1 km/s @ 73 AU
0.36” x 0.33”
0.1” x 0.1”
Lee et al. (2008)
Search for the rotation in the HH211 & HH212 jets
‣ Targets: HH211 & HH212
- The axes of these jets are close to the plane of the sky
➡ suitable for searching the velocity gradient across the jets
‣ Lines: SiO J=8-7, SO NJ=89-78, CO J=3-2
‣ 1 pointing centered at the protostelar positions
‣ Angular resolution: ~ 0.1”
- the jets need to be spatially resolved along their minor axes
Observations with ALMA — 2
Time variability of the jets
HH211 jet in 2004 and 2008
beam size: 1.28” x 0.84”time interval: 3.6 yrsproper motion: ~0.13” ± 0.04” per yeartransverse velocity: 170±60 km/s
The SiO emission from the innermost knot pair has increased
Multi-epoch observations at ~01”resolution
‣ Targets: HH211 & HH212
‣ Lines: SiO J=8-7, SO NJ=89-78, CO J=3-2
‣ 1 pointing centered at the protostelar positions
‣ Angular resolution: ~ 0.1”
‣ proper motion of the HH211 knots (0.13”per yr) can be detectable in 1 yr
‣ 3-epoch observations separated by 1 yr
‣ Variation of the structure of the innermost knots (e.g. new ejection event) is expected
Observations with ALMA — 3
B-field geometry the jets
Polarized CO J=2-1 and dust continuum emission in NGC 1333 IRAS 4
Girart, Crutcher & Rao (1999) Girart, Rao, & Marrone (2006)
B-field measurements using the polarized molecular lines
‣ Targets: HH211 & L1448C
‣ The SiO emission is bright in these sources
‣ Lines: SiO J=8-7, SO NJ=89-78, CO J=3-2
‣ 3--5 pointings (cover the inner ~30”area)
‣ Angular resolution: ~ 0.3”-- 0.5”
‣ Polarization measurements
‣ High dynamic range of >50 is necessary
‣ B-field in the jet v.s. B-field in the disk (from dust continuum observations)
‣ B-field in the jet v.s. B-field in the outflow shell
Observations with ALMA — 4
Search for the highly-
collimated molecular jets in
protostellar outflows
‣ Highly-collimated jet like HH211 is not common‣ Only seen in the extremely young sources
CO J=2-1 outflow from B335
Yen et al. (2010)
Search for the extremely high velocity jet in class 0 protostars‣ Targets: Class 0 protostars without
extremely high velocity jet
‣ First, try to start from B335
‣ Next, go to the various class 0 protostars
‣ Lines: CO J=3-2 or CO J=2-1
‣ 1 pointing centered at the protostelar positions
‣ Angular resolution: ~ 1”
‣ High sensitivity is essential
Near future directions
higher angular resolutiondown to < 0.1”
well studied objects-structure and kinematics near the base-jet rotation?, precession?-proper motion study-time variability study
evolutionary sequence~0.5–1” resolution
outflows in various evolutionary stages-when and how the outflow starts?-when and how the EHV jet develops and disappears?
outflow study with various lines
~0.5–1” resolution-shock chemistry-chemical evolution-which line is suitable for probing the primary ejecta?