Science Briefing August 2, 2018
Understanding the origins and Dr. Emma Marcucci (STScI) Dr. Farisa Morales (JPL) diversity of planets Dr. Hilke E. Schlichting (UCLA)
Facilitator: Dr. Emma Marcucci (STScI) Additional Resources http://nasawavelength.org/list/2240
Resources : Citizen Science: Disk Detective Citizen Science: Exoplanet Explorer1 Active Accretion Learning Game2 Exoplanet Travel Bureau Eyes on Exoplanets (including tutorial video) Exploring Solar Systems Across the Universe
Highlighting the 15th Anniversary of the Spitzer Space Telescope: CoolCosmos - Exoplanets TRAPPIST-1 Products Additional Spitzer resources (images, videos, news releases): http://www.spitzer.caltech.edu/
Press Releases (selected examples) Chandra May Have First Evidence of a Young Star Devouring a Planet First Confirmed Image of Newborn Planet Caught with ESO’s VLT Hubble Gets Best View of a Circumstellar Debris Disk Distorted by a Planet Hubble Directly Observes Planet Orbiting Fomalhaut Spitzer Finds Organics and Water Where New Planets May Grow 2 Outline of this Science Briefing
1. Resources – Greatest Hits
2. Dr. Farisa Morales (JPL) – Exploring Planetary Debris Systems
3. Dr. Hilke Schlichting (UCLA) – Origin and Diversity of Exoplanets
4. Discussion / Questions
3 Resources on Planetary Formation
Disk Detective – Citizen Science Exoplanet Explorers – Citizen Science
Eyes on Exoplanets – Interactive, self-guided exploration
Emma Marcucci Space Telescope Science Institute 4 Disk Detective – Citizen Science originally presented September 2017 by Dr. Marc Kuchner (NASA GSFC)
DiskDetective.org
5 Disk Detective
Informational Buttons
Step 1 – Watch the images
Step 2 – Select descriptor(s)
Step 3 – Finish 6 Exoplanet Explorers – Citizen Science originally presented January 2018 by Dr. Geert Barentsen (NASA Ames) and March 2018 by Dr. Jessie Christiansen (IPAC/Caltech)
ExoplanetExplorers.org
7 Exoplanet Explorers – Citizen Science
8 Exoplanet Explorers Informational Buttons Step 1 – Examine Light Curve
Step 2 – Does it look like the example? Step 3 – Done
9 Eyes on Exoplanets originally presented March 2017 by Carolyn Slivinski (STScI) https://eyes.nasa.gov
10 Eyes on Exoplanets
Explore Buttons
System Information
11 Eyes on Exoplanets
Latest Exoplanet Discoveries missions Home Kepler
View Weird Search from Planets Settings Earth
Different views
Learning through comparison 12 EXPLORING PLANETARY DEBRIS SYSTEMS Please provide: • Title and nice image introducing your topic
Image Credit: NASA/JPL-Caltech Dr. Farisa Morales
13 Stars FormStars with Proto Form-Planetary w/ Disks Protoplanetary Disks Building Planetesimals
http://www.spitzer.caltech.edu/video-audio/730-ssc2004-22v2-The-Evolution-of-a-Planet-Forming-Disk
Dr. Morales 14 Image Credit: NASA/JPL-Caltech A Few Remarks On Dust Planet Perturbations Induce Dust Production Properties
http://www.spitzer.caltech.edu/video-audio/749-ssc2005-10v1-Band-of-Rubble?autoplay=true&limit=100
Dr. Morales 15 Image Credit: NASA/JPL-Caltech EvolutionFormation of aof Planet Rubble Forming Bands Disk
http://www.spitzer.caltech.edu/video-audio/724- ssc2004-17v2-Swirling-Rings-of-Dust
Dr. Morales 16 Image Credit: NASA/JPL-Caltech Exoplanetary Systems
Exoplanet Observations
Debris Disk Observations
Dr. Morales 17 Image Credit: NASA/JPL-Caltech What factors inform us of their architecture? Ultimately, we want to know how they compare to the solar system.
Dr. Morales 18 Summer 2018 SED Modeling – Two Belts (SED = Spectral Energy Distribution)
IRS MIPS
Star Cold Model
Warm
Cold
Warm
Figure 1 Morales et al. (2011)
Dr. Morales 19 Summer 2018 Two Belt Temperatures
Median ~190 K
Figure 2 Morales et al. (2011)
• Dust production is clearly favored at the same characteristic Tdust horizon — across the large stellar spectral range (B8-K0)
— slightly above the ice evaporation temp. for inner belts!
• Note the relative void in Tdust ~ 100 K
Dr. Morales 20 Summer 2018 How does Herschel help clear the picture?
By providing the spatial distribution, we can learn about grain properties
Dr. Morales 21 Summer 2018 Herschel Resolved Outer/Cold Rings! (PSF subtracted Mosaic)
~2” – 5” ~30 – 270 AU
HD 107146 HD 166 HD 38206 HD 61005 HD 70313
N
E HD 104860 HD 10939 HD 159492 HD 138965 HD 71722
HD 153053 HD 141378 HD 192425 HD 28355 HD 30422
Figure 1 Morales et al. (2016)
Dr. Morales 22 Summer 2018 SED Modeling Using Inhomogeneous Particles Are the dust grains rocky or icy?
Dr. Morales 23 Summer 2018 Grain Structures & Composition
• There exists a degeneracy: grain properties vs. radial position Breach degeneracy by considering resolved locations (grain’s position) & and realistic particle properties (homogeneous rocky & inhomogeneous icy)
• Why Icy Particles? – Protostellar sources (Preibisch et al., 1993) – Cometary dust (Kimura et al., 2009) – Kuiper belt objects (KBOs) have distinctly high albedos reflective water-ice particles (Stansberry et al., 2005, Brucker et al., 2009)
A presolar (stardust) grain of silicon carbide, SiC. The grain is only 3 mm across. Photo by Rhonda Stroud, Naval Research Lab., and displayed in Nittler (2003).
Figure 5 Morales et al. (2013)
Dr. Morales 24 Summer 2018 The SED Model
We model each ring as optically thin thermal emission from a series of annuli around the parent star. Dr. Morales 26 Summer 2018 SEDs with Herschel – HD 159492 • The shape of the SED and the fixed radial location suggests that the composition of grains in the outer belt is icy (not rocky) !!
• HD 159492 – A5IV-V, – ~170 Myr – 42.2 pc – fMB= amin/aBOS ≈ ⅓−¼ – Mcold ≈ 0.08 MMoon
Figure 5 Morales et al. (2016)
Dr. Morales 27 Summer 2018 SEDs with Herschel – HD 70313
• Icy grains best fit the shape of the outer dust emission and radial location Spitzer Herschel • HD 70313 – A3V, V = Star – ~300 Myr Model – 51.4 pc – fMB= amin/aBOS ≈ 1 – Mcold ≈ 0.23 Mmoon
Dirty Ice (IMPs) Blackbody
AstroSil
Cold
Warm
Dr. Morales 28 Summer 2018 SEDs with Herschel – HD 166 • HD 166 – K0V – ~456 Myr – 13.7pc – fMB= amin/aBOS ≈ 1 – Lcold ≈ 7.5e-5 – Mcold ≈ 0.009 MMoon
Dr. Morales 29 Summer 2018 In Summary— 6. 5. 4. 3. 2. 1. between? Planets? location. distribution and composition vs. radial modeling; i.e. grain properties, size break the degeneracy RESOLVED modeling dustof at longer dust, and helps presence the of warm and solar excess of emission debris around A GAPS Radial location Some Herschel Spitzer Spitzer — are evident PACS images are spatially IRS well sees both Asteroidal - PACS confirmed the type type main sequence stars. at 100and/or 160 Reveals Water Ice constrain - cold plus plus characterized the warm and cold dust - dustflux Kuiper belt like What’s in in in SED emission. the the l . m 30 help help m . - Summer 2018 Summer Planet Hunting— an ongoing effort Do they look like us?
Dr. Morales 31 Summer 2018 Planet Hunting NASA-Keck II Observatory (2012 – present)
Dr. Morales 32 Summer 2018 Planet Hunting NASA-Keck II Observatory (2012 – present)
Dr. Morales 33 Summer 2018 Adaptive optics -- Gemini Observatory
https://www.youtube.com/watch?v=CyGRLr9H1x4
Dr. Morales 34 Summer 2018 Dr. Morales 35 Summer 2018 Dr. Morales 36 Summer 2018 Thank You!
37 Image Credit: NASA/JPL-Caltech Origin and diversity of Exoplanets
Prof. Hilke Schlichting (UCLA) 38 Kepler Planets
4496 Planetary Candidates 1218 Planets in Multi-Planet Systems
39 Kepler Planets
4496 Planetary Candidates 1218 Planets in Multi-Planet Systems
40 Kepler Planets
4496 Planetary Candidates 1218 Planets in Multi-Planet Systems
41 Fressin 2013
42 43 NASA/JPL-Caltech Exoplanet Atmospheres
Lopez, 2013, Lopez et al.2012
For comparison, the Earth’s atmosphere contains less than 10-6 of its mass and has an atmospheric scale height that is only ~ 0.1% of its radius. 44 Exoplanet Densities
20 15 (b) 10
5
]
3
m c 2
=
g
[
; 1
0.5
0.2 1 1.5 2 3 5 7 10 15 20 Giant Impacts can strip the M ass [M ) ] atmosphere of exoplanets leading to a Inamdar & Schlichting 2016 diversity in compositions
Data from Weiss & Marcy 2014, Juntof-Hutter et al. 2015, Barros et al. 2015 45 Exoplanet Densities
20 15 (b) 10
5
]
3
m c 2
=
g
[
; 1
0.5
0.2 1 1.5 2 3 5 7 10 15 20 Giant Impacts can strip the M ass [M ) ] atmosphere of exoplanets leading to a Inamdar & Schlichting 2016 diversity in compositions
Data from Weiss & Marcy 2014, Juntof-Hutter et al. 2015, Barros et al. 2015 46 Exoplanet Densities
20 15 (b) 10
5
]
3
m c 2
=
g
[
; 1
0.5
0.2 1 1.5 2 3 5 7 10 15 20 Giant Impacts can strip the M ass [M ) ] atmosphere of exoplanets leading to a Inamdar & Schlichting 2016 diversity in compositions
Data from Weiss & Marcy 2014, Juntof-Hutter et al. 2015, Barros et al. 2015 47 Exoplanet Densities
20 15 (b) 10
5
]
3
m c 2
=
g
[
; 1
0.5
0.2 1 1.5 2 3 5 7 10 15 20 Giant Impacts can strip the M ass [M ) ] atmosphere of exoplanets leading to a Inamdar & Schlichting 2016 diversity in compositions
Data from Weiss & Marcy 2014, Juntof-Hutter et al. 2015, Barros et al. 2015 48 Take Home Points
1) Super-Earths & Mini-Neptunes are the most abundant planets known to date in our galaxy
2) About 50% of stars have a close-in Exoplanet larger than Earth in size.
3) About 10% of stars have a ‘Jupiter’.
4) Small number of Giant Impacts can give rise to a large diversity in exoplanet densities. Explanation for diverse bulk densities observed in multiple planet systems: e.g. Kepler-11, Kepler-20, Kepler-36, Kepler-48, and Kepler-68
49 To ensure we meet the needs of the education community (you!), NASA’s UoL is committed to performing regular evaluations, to determine the effectiveness of Professional Learning opportunities like the Science Briefings. If you prefer not to participate in the evaluation process, you can opt out by contacting Kay Ferrari
This product is based upon work supported by NASA under award number NNX16AC65A to the Space Telescope Science Institute, working in partnership with Caltech/IPAC, Jet Propulsion Laboratory, Smithsonian Astrophysical Observatory, and Sonoma State University. Any opinions, findings, and conclusions or recommendations expressed in this material are those of the author(s) and do not necessarily reflect the views of the National Aeronautics and Space Administration.
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