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ESO Herbig Ae/Be Workshop���(Faulty) Summary

Nuria Calvet University of Michigan

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1992 Conference in Amsterdam

Disks or Envelopes? Hillenbrand et al. 1992 Massive circumstellar disks

Near-IR “bump” at ~ 2.2-3 µm, Rhole ~ 3-25 R*

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Dust sublimation radius

Emission from inner disk wall Natta et al 2001; Tuthill et al. 2001

Kraus

Evidence for a puffed-up inner rim: Imaging

Benisty et al. 2011, Kluska et al. 2014 also: Renard et al. 2010; talk today by J. Kluska

Image after removing the photospheric contributions

Image after removing photospheric and inner disk contributions

J. Kluska - IPAG - Imaging of YSO

−5 0 5

−5

0

5

0.0e+00

3.3e−04

6.6e−04

9.9e−04

1.3e−03

1.7e−03

2.0e−03

2.3e−03

2.7e−03

3.0e−03

3.3e−03

Δα (mas)

Δδ

(mas

)

HD144432 − f 0.4 − d 1.0

HD144432

Images from HAeBe survey PIONIER

08/04/2014 J. Kluska - IPAG - Imaging of YSO 5

−5 0 5

−5

0

5

0.0e+00

2.7e−04

5.4e−04

8.1e−04

1.1e−03

1.4e−03

1.6e−03

1.9e−03

2.2e−03

2.4e−03

2.7e−03

Δα (mas)

Δδ

(mas

)

HD142527 − f 0.45 − d 1.0

HD142527 −10 0 10

−10

0

10

0.0e+00

6.0e−05

1.2e−04

1.8e−04

2.4e−04

3.0e−04

3.6e−04

4.2e−04

4.8e−04

5.4e−04

6.0e−04

Δα (mas)

Δδ

(mas

)

HD98922

−10 0 10

−10

0

10

0.0e+00

6.0e−05

1.2e−04

1.8e−04

2.4e−04

3.0e−04

3.6e−04

4.2e−04

4.8e−04

5.4e−04

6.0e−04

Δα (mas)

Δδ

(mas

)

HD100546

−10 0 10

−10

0

10

0.0e+00

7.5e−05

1.5e−04

2.2e−04

3.0e−04

3.7e−04

4.5e−04

5.2e−04

6.0e−04

6.7e−04

7.5e−04

Δα (mas)

Δδ

(mas

)

−5 0 5

−5

0

5

0.0e+00

2.2e−04

4.4e−04

6.6e−04

8.8e−04

1.1e−03

1.3e−03

1.5e−03

1.8e−03

2.0e−03

2.2e−03

Δα (mas)

Δδ

(mas

)

HD37806 − f 0.21 − d 1.0HD37806 − f 0.28 − d 1.0

HD37806

Bpshe

A9Ve

B9Ve

A2Vpe

B9e

F0IIIe F6IIIe

B0 B9Vne

−5 0 5

−5

0

5

0.0e+00

2.8e−04

5.5e−04

8.3e−04

1.1e−03

1.4e−03

1.7e−03

1.9e−03

2.2e−03

2.5e−03

2.8e−03

Δα (mas)

Δδ

(mas

)

HD158643 − f 0.9 − d 1.0

HD158643

A0V

−10 0 10

−10

0

10

0.0e+00

6.5e−05

1.3e−04

2.0e−04

2.6e−04

3.3e−04

3.9e−04

4.6e−04

5.2e−04

5.9e−04

6.5e−04

Δα (mas)

Δδ

(mas

)

HD50138

−20 0 20

−20

0

20

0.0e+00

6.0e−05

1.2e−04

1.8e−04

2.4e−04

3.0e−04

3.6e−04

4.2e−04

4.8e−04

5.4e−04

6.0e−04

Δα (mas)

Δδ

(mas

)

HD45677

−10 0 10

−10

0

10

0.0e+00

1.0e−04

2.0e−04

3.0e−04

4.0e−04

5.0e−04

6.0e−04

7.0e−04

8.0e−04

9.0e−04

1.0e−03

Δα (mas)

Δδ

(mas

)

MWC297

−10 0 10

−10

0

10

0.0e+00

1.0e−04

2.0e−04

3.0e−04

4.0e−04

5.0e−04

6.0e−04

7.0e−04

8.0e−04

9.0e−04

1.0e−03

Δα (mas)

Δδ

(mas

)

HD100453

Kruska, Thi

NIR MIR sub-mm

Multi-wavelength interferometry

near-infrared

NIR/MIR/mm wavelength regimes…

..trace different disk radii

…trace disk surface & interior

Menu MIDI survey

Mid IR analysis of SEDs implies asymmetries: Jamialahmadi

Gas diagnostics: CO lines

Brittain

Van der Plas

Some transitional disks – disks with inner disk clearings- (i.e HD100546), seem to have non molecular inner regions, ≥ 10 au (Brittain, van der Plas) Width of profiles consistent with formation within ~ 2au in HD 163296, HD250550, Hen 2-80 (Bertelsen) Need survey of sources with different SEDs

Gas diagnostics: CO lines

PACS + Spires: CO ladder Groups I flared gas disks A few Group II Menard, Meeus, Woitke Scale height at 100 AU to explain low J CO (Pietu) higher than dust scale height (Grady) Difficult to explain bright [OI] Few sources analyzed, need more to draw general conclusions

Very elaborated models, difficult to get general physical conclusions Woitke, Pinte

Other gas diagnostics

No hot H2O – unlike CTTS OH most common Warm H2O

Fedele: hotter disks in HAe

Great things to be done by SOFIA Zinnecker

H2O dependendence on dust/gas Antonellini

All Group I have gaps?

model:!wall at 34 au

Q-band!!!

HD97048

PSF

Maaskant et al. 2013,!Khalafinejad et al. 2014!

!• Connection SEDs,

gaps and absence of silicate features. !

• New simple Meeus group classification based on F30/F13.5 ratio

example:

2.1 5.1

filled symbols have gaps

Group I morphologies

All Group I have SED consistent with being pre-transitional: Disks with gaps with inner optically thick material

Grady

Gap diagnostics: PAH

Maaskant

Gaps/Arms/Asymmetries due to planet formation?

Polarimetric Differencial Images Quanz

Planet formation?

Line asymmetries in HD 100546 caused by companion in excentric orbit

Brittain

Gaps/Arms/Asymmetries due to planet formation?

Van der Marel

Gaps/Arms/Asymmetries due to planet formation?

Van der Marel

Gaps/Arms/Asymmetries due to planet formation?

Van der Marel Transitional disks may be dust traps indicating planet formation - ALMA

Gaps/Arms/Asymmetries due to planet formation?

Menard, Perez, Casassus, Christiaens

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Evolution

IM protostars form as low mass protostars. Disks and collimated outflows with similar properties to low mass protostars (Beltran, Wu, Comeron) Jets in Herbig rare but selection effect but similar to low mass protostar (Dougados). Soft X-rays from jets (Schneider) Reiter

HD163296 Ellerbroek et al. 2014

Comeron

All molecular outflows are collimated (Beltran, Dougados) and jets can produce (soft) cosmic rays (Ray)

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Evolution

Wyatt

Pristine or secondary dust in TD? Fe-rich dust in warm debris disk (Henning) Compare to PPD – 10 mm spectroscopic studies (Boekel, Vieria)

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Evolution of gas

Wyatt

β Pic gas is secondary Dent

30 Myr old HD 21997: gas primordial Kospal

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Disk evolution in clusters

Yasui

Longer lifetime for mid-IR disk

Lifetimes shorter in IM than in LM (Yasui) Mechanism not understood (Kunimoto)

Z-dependence of mass accretion rate (Beccari)

Searches Ae/Be in the LMC (Mathew) Fe/Ge in Ori OB1 (Hernandez)

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Binaries

Rodgers

For every star there is a companion at some separation Duchene

Also Briceno Csepany

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Accreting? How?

Hillenbrand et al. 1992 Massive circumstellar disks 6x10-7 < Mdotacc < 8x10-5 Msol/yr Accreting? What are the mass accretion rates?

Grady et al. (1996)

HD100546

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Magnetospheric Accretion: shock emission Excess due to shock emission to estimate mass accretion rates

Warning: excess very dependent on spectral type

Mendigutia

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Magnetospheric Accretion: shock emission

Fairlamb Large X-shooter study

Extend relation from brown dwarfs to CTTS to Herbig Ae MA does not fit strong UV excess in early B stars Also Vink

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Calibration of line indicators Mendigutia, Fairlamb Warning: Not all work:

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Support MA Vink Linear Polarization Rotating disk geometry Similar for HAeBe and CTTS Inner disk radius

Many (statistics?) H line profiles consistent with MA Brittain, Arnio, Ramirez, Gotzens, Van den Ancker Although few redshifted absorptions, and some extended

Kraus Compact Brγ emitting region in most low L sources

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Against MA: weak/absent magnetic fields Alecian 128 stars, 1.5-20 Msun 8 stars detected (6%) strong Others ≤ 100 G

Hussain IMTTS, dipole component gets weaker with increasing radiative core

Also Petr-Gotzens, Ababakr

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Question: Where does the excess come from? Boundary layer? MA profiles Inner gas disk? Too cold?

Ilee

Kraus Dougados

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Hot inner disk?

Brittain

Kratter, Lobato

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Summary of the summary Ø  Images: New view on the nature of disks around Herbig Ae/Be Ø Group I may all have cavities/gaps and outer disks are very

structured Ø Need statistics Ø Generalized dust traps may indicate planet formation Ø Are early Be to be included in the class? Ø  Stars are accreting – excess, outflows – but weak, multipolar

magnetic fields Ø How are they accreting? Ø Great conference!

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And don’t forget

au AU