Synoptic Observations of Young Starswith Planet-Building Disks

IRTF Workshop 2018

Mike Sitko (U Cincinnati & Space Sci. Inst.) Monika Pikhartova (U Cincinnati)

Carol Grady (Eureka Scientific, Inc.) John Wisniewski (U Oklahoma)

Evan Rich (U Oklahoma)

SCHEDULING!

DIAGNOSTICS - gas & DUST

IRTF Workshop 2018

2003 - inner rim was 20% bigger!

– 11 –

-0.4 -0.2 0.0 0.2 0.4AU

-0.4

-0.2

0.0

0.2

0.4

’Standard’ inner-rim model (K band image)

0.07

0.11

0.15

0.19

0.23

0.27

(Sur

face

Brig

htne

ss (e

rg/s

/cm

^2) )

^0.1

-0.6 -0.4 -0.2 0.0 0.2 0.4 0.6AU

-0.6

-0.4

-0.2

0.0

0.2

0.4

0.6

’Standard’ inner-rim + gas model (K band image)

0.07

0.10

0.14

0.18

0.21

0.25

(Sur

face

Brig

htne

ss (e

rg/s

/cm

^2) )

^0.1

Fig. 1.— Representative models for near-IR emission in Herbig Ae stars. a) Left panel. A

standard curved dust-rim-only model (Isella & Natta 2005; Tannirkulam et al. 2007) wherethe dust sublimation temperature is a power-law function of gas density (Pollack et al. 1994).b) Right panel. Gas emission (modeled as a uniform disk centered on the star) has been

added inside the dust rim in order to smooth out the emission profile.

resolved inner gas

Adapted (and embellished) from Tannirkulam et al. 208, ApJ, 677, L51

IRTF Workshop 2018

Wisniewski et al.2008, ApJ, 682, 548

IRTF Workshop 2018

HD 163296 = MWC 275

Increased disk wall height - increased near IR flux - causes increased shadowing and drop in mid-IR flux ("see-saw")

LRLL 31 - Muzerolle et al. 2009

Ellerbroek et al. 2014, A&A, 563, A87

IRTF Workshop 2018

IR only sparsely sampled

IRTF Workshop 2018

Periodic HH Knots ~16 year photometric periodProper motion traceback

HD 163296 = MWC 275

Ellerbroek et al. 2014, A&A, 563, A87

IRTF Workshop 2018

jet thermal emission

middle disk no longer shadowedV band drop

from Monika Pikhartova et al. AAS 2017 & 2018

MCRT Model

jet blocks direct illumination by star

IRTF Workshop 2018

What Next?Coordinate with Interferometers (again)Already did this with Keck (no longer KI) & VLTI/MATISSE (mid-IR 4T)Discussed with CHARA Director and 6T Scientists Monnier last year

Kraus et al. 2013

Millan-Gabet et al. 2016

MWC 480 CHARA 6T

IRTF Workshop 2018

What Next?Support of JWST (& other Coronagraphs) - What IS the illumination of thedisks? (bright stars observable with JWST/MIRI coronagraph, NIRISS-SAM)

SAO 206462(Muto et al. 2012)

MWC 480 (Kusakabe et al. 2012)

IRTF Workshop 2018

What Next?

Return of MIRSI with Visible-Wavelength (Guider) Capability and Extension to mid-IR - variability, including “see-saw” behavior, daytime observing

SpeX

MIRSI

?