high resolution sub millimetre studies of the chemistry of low mass protostars
Download
Skip this Video
Download Presentation
High resolution (sub)millimetre studies of the chemistry of low-mass protostars

Loading in 2 Seconds...

play fullscreen
1 / 27

High resolution (sub)millimetre studies of the chemistry of low-mass protostars - PowerPoint PPT Presentation


  • 122 Views
  • Uploaded on

High resolution (sub)millimetre studies of the chemistry of low-mass protostars. ...or “where did all the CO go?”. Jes J ø rgensen (CfA) Fredrik Sch ö ier (Stockholm), Ewine van Dishoeck (Leiden), Michiel Hogerheijde (Leiden), Geoff Blake (Caltech) Tyler Bourke, David Wilner, Phil Myers (CfA).

loader
I am the owner, or an agent authorized to act on behalf of the owner, of the copyrighted work described.
capcha
Download Presentation

PowerPoint Slideshow about ' High resolution (sub)millimetre studies of the chemistry of low-mass protostars' - hayes-fuentes


An Image/Link below is provided (as is) to download presentation

Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author.While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server.


- - - - - - - - - - - - - - - - - - - - - - - - - - E N D - - - - - - - - - - - - - - - - - - - - - - - - - -
Presentation Transcript
high resolution sub millimetre studies of the chemistry of low mass protostars

High resolution (sub)millimetre studies of the chemistry of low-mass protostars

...or “where did all the CO go?”

Jes Jørgensen (CfA)Fredrik Schöier (Stockholm), Ewine van Dishoeck (Leiden), Michiel Hogerheijde (Leiden), Geoff Blake (Caltech)Tyler Bourke, David Wilner, Phil Myers (CfA)

ACP

Cardiff, January 6th 2005

low mass star formation
Low-mass star formation

Pictures from NASA/Astronomical picture of the day; Myers et al. (1998)

protostellar properties
Protostellar properties
  • Centrally condensed envelope of gas and dust
  • Ongoing accretion through a circumstellar disk
  • Densities ranging from 104 cm-3 to 107-108 cm-3 (H2)
  • Temperatures ranging from 10 to a few hundred K.
this study
This study

Establish the physical and chemical structure of a sample of ~ 20 low-mass protostars (class 0/I); using single-dish obs. (JCMT), mm interferometry and detailed radiative transfer modeling.

  • What is the relation between the physical and chemical properties of low-mass protostars?
  • What are the useful diagnostics of different protostellar components?
  • Is it possible to use the chemistry to trace the protostellar evolution?
approach

SCUBA obs. + Rad. transfer model.

Single-dish obs. + Monte Carlo model.

Approach

Dust continuum emission

  • CO
  • CS, SO
  • HCO+, N2H+
  • HCN, HNC, CN
  • DCN, DCO+
  • H2CO, CH3OH
  • SO2, SiO, H2S, CH3CN(~ 40 transitions)

Physical structure

Molecular excitation

Chemical structure

Detailed chemical model

Interferometry:small scale structure

today
Today...

...very little about continuum observations and dust radiative transfer

BUT: Continuum/Physical structures...

  • ...describe star formation/core physical evolution
  • ...are crucial for molecular excitation calculations
  • ...establish reference scale (H2 density) relative to which abundances are calculated
  • ...include significant simplifying assumptions (e.g., dust properties, dust-gas coupling...)
slide8

Example: modeling of CO lines toward L723

Adopting n(r) and T(r) from continuum modeling: constrain abundances (and velocity field) from Monte Carlo line radiative transfer by comparison to observed line profiles.

slide9

“Canonical” CO abundance (Lacy et al. 1994)

CO depletion

CO freezes out at low temp. ( 35 K) - as seen in pre-stellar cores (e.g., Caselli et al. (1999), Tafalla et al. (2002))

Objects with high envelope masses (younger?) show significantly higher degree of CO depletion

Jørgensen, Schöier & van Dishoeck 2002 A&A, 389, 981

slide10

Abundance

  • Pre-stellar core:
  • Low temperature
  • Depletion toward center (high densities ~ time)
  • ...but not edge
  • Protostellar core:
  • Central heating ~ temperature gradient
  • Thermal desorption toward center
  • ...outside (low T): depletion/no depletion regions as in pre-stellar stages

Caselli et al. (1999), Tafalla et al. (2002), Bergin et al. (2002), Bacmann et al. (2002), Lee et al. (2003)...

Jørgensen, Schöier & van Dishoeck, 2005, A&A submitted

slide12

L723:

Constant abundance model

“Drop” abundance model

slide14

Depletion ~ Time

( 105 yrs)

  • “Drop abundance structure” needed to account for both single-dish and interferometer observations
  • Explains differences in CO abundances between YSOs with envelopes of different masses- but note: no trend between tde and “age”
  • Potentially(!) a tracer of the “history” of the core- dense stage (where CO depletes) only 105 years?
slide16

Empirical chemical network

CO

CS

HCO+

SO

CN

HNC

HCN

HC3N

Jørgensen, Schöier & van Dishoeck 2004, A&A, 416, 603

slide17

dust grains

CO

H3+

HCO+

N2

N2H+

hco and n 2 h abundances
HCO+ and N2H+ abundances

Jørgensen, Schöier & van Dishoeck 2004, A&A, 416, 603

slide19

CO freeze-out X(N2H+)

CO desorption (T> 30 K)

L483:

“Typical embedded pro-tostar (quite asymmetric, though) at a distance of approximately 200 pc.”

 450 m dust continuum

 N2H+J = 10

 C18O J = 10

1” = 200 AU  3×1015 cm

Jørgensen, 2004, A&A, 424, 589

slide20

L483:

“Typical embedded pro-tostar (quite asymmetric, though) at a distance of approximately 200 pc.”

 450 m dust continuum

 N2H+J = 10

 C18O J = 10

1” = 200 AU  3×1015 cm

Jørgensen, 2004, A&A, 424, 589

chemistry as a tool
Chemistry as a tool...

NGC 1333-IRAS2

SCUBA 850 µm

BIMA: N2H+ 1-0*

chemistry as a tool1

2C

2A

2B

Dashed line: SCUBA continuum emissionSolid line: Contrast N2H+/SCUBA emission

Chemistry as a tool...

NGC 1333-IRAS2

BIMA: N2H+ 1-0*

Jørgensen, Hogerheijde, van Dishoeck et al., 2004, A&A, 413, 993

slide23

Depletion ~ Time

( 105 yrs)

chemistry as a tool2

2C

2A

2B

Time

Dashed line: SCUBA continuum emissionSolid line: Contrast N2H+/SCUBA emission

Chemistry as a tool...

NGC 1333-IRAS2

BIMA: N2H+ 1-0*

Jørgensen, Hogerheijde, van Dishoeck et al., 2004, A&A, 413, 993

slide25

dust grains

CO

H3+

HCO+

N2

N2H+

Previously N2 assumed to freeze-out slower than CO(e.g., Bergin & Langer, 1997)– but recent observations show N2H+ depleting towards the centers of pre- and protostellar cores (although slower than CO)(e.g., Bergin et al. (2002), Belloche & André (2004))and lab. experiments show similar binding energies for CO and N2(Öberg et al.)

?

co hco n 2 h
CO-HCO+-N2H+

BLACK/BLUE: [CO] varying

RED:[CO] & [N2] varying

Chemistry of gas parcel at 106 cm-3 and 20 K after 104 years following model of Doty et al. (2004) with varying CO – and N2 - depletion

conclusions
Conclusions

A quantitative framework for the interpretation of the detailed physical and chemical structure of early protostellar sources has been established.

  • Continuum emission; dust radiative transferPhysical structure of envelopes (down to 500 AU) (The presence or absence of disks)
  • Molecular line studiesChemical evolution ~ thermal history (e.g., CO)
  • Important link between high-resolution observations, single-dish surveys and detailed modeling
ad