Yso pms disk types time scales and evolution
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YSO/PMS disk types, time-scales and evolution. Luke Thomas Maud – ESAC Trainee 2009 Bruno Merin – Herschel Science centre (Supervisor) ‏ Herv é Bouy – Herschel Science centre (Research Fellow). Outline. Formation Scenario The Sample Spectra Categorization Mass and Age Estimates Results

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Yso pms disk types time scales and evolution
YSO/PMS disk types, time-scales and evolution

  • Luke Thomas Maud – ESAC Trainee 2009

  • Bruno Merin – Herschel Science centre (Supervisor)‏

  • Hervé Bouy – Herschel Science centre

    (Research Fellow)


Yso pms disk types time scales and evolution

Outline

  • Formation Scenario

  • The Sample

  • Spectra

  • Categorization

  • Mass and Age Estimates

  • Results

  • Conclusion and Possible Interpretation

  • The Future


Yso formation

Using IR we can probe clouds and ‘see’ YSOs inside:

YSO Formation

  • Young stellar objects form in molecular clouds, opaque to optical light

  • Clouds collapse, cores form..

  • Angular momentum conservation generates a spinning disk as material falls inwards..

  • As the disks evolve they disperse/evaporate and the central star joins the main sequence...

  • It is possible that a planetary system is created.


Formation spectral energy distributions
Formation – Spectral Energy Distributions

  • Since the late 80s investigations have been undertaken to evaluate the evolution of YSOs

  • Adams, Lada and Shu 1987 developed the ‘classical’ classification system for YSOs

  • Using Spectral Energy Distributions (SEDs) one can see how the flux of the emission varies

  • Thus how the YSO evolves

  • This however is the ‘general’ model and classes are based upon a slope from 2 to 24 um wavelengths


The sample

IC 348 Perseus

Rho Ophiuchus

NGC 1333 Perseus

Serpens Core

The Sample

  • This project is a continuation of previous papers investigating the 5 close star forming regions from the Cores to Disks (c2d) Spitzer legacy program (Evans et al 2009)

  • The initial sample had photometry for 1024 YSO candidates with estimated ages of 1 -10 Myrs

  • Encompassing the timescales of disk dissipation previously observed for low mass stars and probing slightly different environments


The sample1
The Sample

  • However after analysis, the C2D YSOs had unexplainable age attributes

  • The problem is due to the degeneracy involved in SED fitting

  • We created a new sample of objects that had full spectroscopic data, this means the Spectral types of the stars could be constrained

  • We include only stars that are Class II and III from (Greene et al. 1994)‏

  • II -1.6 ≤ α < -0.3, III α < -1.6

  • We now have a fully usable sample of 819 YSOs


Spectra energy distributions spectra
Spectra Energy Distributions – (Spectra)

  • For all the targets in the sample we create SEDs

  • Thus we plot the wavelength of photometric data vs. the flux at that wavelength


Classification
Classification

  • In comparison to the basic Class II and III we see a more diverse range of SEDs:


Classification1
Classification

So we define limits of classification with reference to the median CTTS and the fitted photospheres


Mass and age estimates
Mass and Age Estimates

  • We get temperatures from the spectral types and luminosities from the fitted photospheres

  • These are passed to HR diagrams for plotting against PMS tracks computed be Baraffe et al (1998) and Siess et al (2000)

  • Sanity check that we are not doing anything ‘silly’ as the objects fit on the HR diagram.


Mass and age estimates1

Mass and Age Estimates

  • We group the objects into 4 groups now

  • Under Luminous – Sources below the tracks – Need to be further away

  • Over-Luminous – Sources above the tracks – Need to be closer

  • Strange – Objects with non-fitting and ‘weird’ SEDs – Would require extra analysis

  • Final – Objects used in the main results – 664


Results
Results age constraints from the HR fitting:

  • The resultant mass and age spread is sensible, and within expected values for Low mass star forming regions:

  • We appear to represent stellar masses down to ~0.03Mo and up to ~ 3.5 Mo


Results1
Results age constraints from the HR fitting:

  • We divide the final group in Mass ranges of:

    • M < 0.5 Mo, 0.5 < M < 1.5 Mo and M > 1.5Mo

  • Separating the stars’ physical properties

    • Fully convective, radiative core/convective envelope and convective core/radiative envelope respectively

  • And Age ranges of:

    • 1 – 5 Myrs, 5 – 10 Myrs and 10 – 20 Myrs

  • To cover the general disk dispersal time scales and evolution

  • We produce 9 pie charts rich with information


Conclusions interpretation
Conclusions - Interpretation age constraints from the HR fitting:

  • The Spitzer data allows the new categorization of the evolutionary stages of disks around YSOs via SEDs and clearly detects ‘transitionals’

    • Largest statistical sample 3-5x bigger than any previous and covers a larger range of ages and environments

  • Initial stages all appear the same (fisher test) – NEW RESULT!

  • More massive stars remove there disks faster, none are present after 10 Myrs

  • Primordial class disks are still evident at ages above 10 Myrs for stars with M < 1.5Mo

  • Mass plays a role in evolution – Has been suggested but this is evidence!

Speculation

  • As it appears that disks around lower mass stars last longer

    • more time for instabilities and coagulation of particles

    • potential home for rocky planets?

  • The most massive stars’ disks disperse fast

    • timescales preferential for large ‘Jupiter’ planets that form over short times in rich disks (we need disk mass)

  • Latest statistics (Udry et al. 2007) suggest low mass stars have low mass multiple planet systems while high mass show single migrated Jupiter mass ones (obviously still limited in technology)


Future
Future age constraints from the HR fitting:

  • The age constrains are the current best with simple HR fitting, however do not account for accretion luminosity and a more robust method is required

    • (under-luminous if not accreting = older)

  • To calculate disk mass we require observations extending into the sub-mm

    • Herschel will provide this coverage and add a new perspective allowing comparisons of disk and stellar mass. One of the key parameters of the disk itself

  • Our method is applicable to the Gould belt clouds currently underway

    • With a much large sample

  • High resolution spectroscopy would help identify transitional disks

    • Binaries are ‘empty’ vs. planet harbouring disks

  • Alma and JWST will shed extra light on the data with increased sensitivity/resolution

    • Imaging will allow disk radii to be constrained


Thank you for your attention any questions please
Thank You for your attention age constraints from the HR fitting:Any Questions Please


A problem scaling
A Problem? - Scaling age constraints from the HR fitting:

  • Note the ranges probed by the photometry (MIPS1)

  • F/A type at ~ 21AU

  • Solar type at ~ 7 AU

  • Low-mass at ~ 3 AU

  • The previous assumptions assume the disks scale with mass and are all comparable – however they may not scale directly (1:1)

  • Thus for are low mass sources in the pie charts classified using a different range in the SEDs??


Scaling
Scaling age constraints from the HR fitting:

  • NO, due to the nature of SED with the logarithmic scale we see only a small shift of data points

  • This would therefore supports that stars and disk may scale together as one may expect (more mass, more gravity, more disk)


Additional classification
Additional Classification age constraints from the HR fitting:

  • To move allow another perspective independent of the larger fluctuation of age in HR fitting; we also present a model based upon the scheme of Cieza et al (2007)

  • Cieza use l turnoff and α excess – which describe the distance of the inner disk to the central star and the degree of opacity or thickness of the disk

  • These are grouped for the same masses as the pie charts


Additional results
Additional Results age constraints from the HR fitting:

  • The ranges of the 3 mass groups appear to be comparable

  • Suggests the actual evolutionary sequence maybe the similar independent upon mass

  • Note the tight range of Primordial disk, with Transitional disks above α = 0 and Settled moving right and down

  • Again the aforementioned ‘scaling’ problem is dismissed as one would expect the turn-off ranges to be altered, but clearly they are similar