1. Disks Around Young Stars with ALMA & SPHEREx
Catherine Espaillat
Boston University

2. Disks Around Young Stars with ALMA & SPHEREx
Submm/mm observatories provide information on the distribution of gas and (large) dust grains in the disk.
SPHEREx can provide complementary information on the innermost disk by
measuring the location, curvature, and height of the inner rim
detecting changes in the inner rim with time

3. Our current sketch of a protoplanetary disk
Henning & Semenov 2014

4. Spatial distribution of dust grains varies with wavelength
TW Hya
Andrews et al. 2012, 2015

5. also AB Aur (Pietu et al. 2005), TW Hya (Hughes et al. 2007),
Several disk cavities now confirmed via submm interferometric imaging
also AB Aur (Pietu et al. 2005), TW Hya (Hughes et al. 2007),
SAO (Brown et al. 2009), RY Tau (Isella et al. 2010a), DM Tau (Andrews et al. 2011),
IRS 48 (Brown et al. 2012), HD (Casassus et al. 2013), Sz 91 (Tsukagoshi et al. 2014)
Figure from Espaillat et al. 2014, PPVI; Data from Mathews et al Isella, et al. 2010, Brown et al. 2009, Andrews et al. 2009, Hughes et al. 2009, Andrews et al. 2011b, Brown, et al. 2008, Cieza et al. 2012, Rosenfeld et al. 2013, Andrews et al. 2010

6. Gas seen within dust cavities with ALMA
van der Marel et al. 2015

7. Striking small-scale disk structure revealed by ALMA
ALMA Partnership 2015

8. Disks Around Young Stars with ALMA & SPHEREx
Submm/mm observatories provide information on the distribution of gas and (large) dust grains in the disk.
SPHEREx can provide complementary information on the innermost disk by
measuring the location, curvature, and height of the inner rim
detecting changes in the inner rim with time

9. NIR excess emission can be used to measure location of inner disk rim
Twall=1400K
Twall=1300K
Twall=1200K
Twall=1000K
Twall=1400K
Muzerolle et al. 2003
Espaillat et al. 2008

10. NIR excess emission can be used to measure shape & height of inner disk rim
Millan-Gabet et al. 2016

11. SPHEREx will provide spectra for every known, nearby YSO
6 arcsec at ~140 pc is ~800 AU
Typical disk is ~600 AU in diameter
SPHEREx will provide spectra for at least 600 disks
Ribas et al. 2014

12. Disks Around Young Stars with ALMA & SPHEREx
Submm/mm observatories provide information on the distribution of gas and (large) dust grains in the disk.
SPHEREx can provide complementary information on the innermost disk by
measuring the location, curvature, and height of the inner rim
detecting changes in the inner rim with time

13. Spitzer IRAC [3.6] and [4.5] YSO Variability Surveys:
Young stellar objects are highly variable
Spitzer IRAC [3.6] and [4.5] YSO Variability Surveys:
Orion Nebula Cluster – YSOVAR (Morales-Calderon et al. 2011)
2000 objects observed 81 times over 40 days
IC 348 (Flaherty et al. 2013)
200 objects observed 38 times over 40 days
IR variability of typically mag seen in ~80% of embedded disk systems, 60-70% of disk systems, and 20-45% of diskless stars.

14. broken line: model with shorter inner rim
Evidence for changes in inner disk rim height via variable “see-saw” IR emission
UX Tau A
broken line: model with shorter inner rim
Espaillat et al. 2011; also Muzerolle et al. 2010, Flaherty et al. 2012

15. Potential causes of changes in inner disk rim height
Planet-disk interaction
Ogilvie & Lubow 2002
Flaherty et al. 2011
Turbulence from MRI
Warped inner disk
Hirose & Turner 2011
Flaherty et al. 2011

16. Disks Around Young Stars with ALMA & SPHEREx
Submm/mm observatories provide information on the distribution of gas and (large) dust grains in the disk.
SPHEREx can provide complementary information on the innermost disk by
measuring the location, curvature, and height of the inner rim
detecting changes in the inner rim with time

17. FUV-NIR variability in disks around young stars
GM Aur
FUV
NUV
Optical
NIR
Ingleby, Espaillat et al. 2015