Science Briefing September 7, 2017

Beyond the Solar System: Dr. Bonnie Meinke (Space Telescope Science Institute) Dr. Rachel Akeson (Infrared Processing and Analysis Center) Cosmic Disks Dr. (NASA Goddard Space Flight Center)

Facilitator: Dr. Brandon Lawton (STScI) Additional Resources http://nasawavelength.org/list/1891

News and Images:  Astronomers Discover an Super Saturn  Giant Ring Discovered around Saturn  Images: Protoplanetary Disks in the Orion Nebula

Citizen Science:  Disk Detective – Featured Activity

Activities:  Building Perspectives with Active Galaxies (1/3)  Zooming in on Active Galaxies (2/3)  Light Travel Time and the Size of Active Galaxies (3/3)  Graphic Organizer: Galaxy Types Compared

2 Our Backyard Laboratory for Disks: Saturn’s Rings

Bonnie Meinke

3 Outer Solar System

4 Planetary Rings

Uranus, as observed by Hubble Saturn, as observed by Hubble 5 Planetary Rings

6 Planetary Rings

7 Planetary Rings

8 Planetary Rings

9 Planetary Rings

10 Planetary Rings

11 Planetary Rings

12 Saturn’s Rings

13 Image credit: NASA/JPL Saturn’s Rings

Broad, dense rings Dusty components

Gaps moons

14 Image credit: NASA/JPL Saturn is a Ring-Moon system!

That means moons and rings interact in a cosmic dance

15 Enceladus

Plume

Feeds the E ring

16 Image credit: Cassini ISS Iapetus

Back/trailing side

Front/leading side

Image credit: Cassini ISS 17 Saturn’s Rings

18 Image credit: NASA/JPL Moons create structure in rings

• Mimas resonance builds structure, both vertical and density enhancements

ISS image 19 Saturn’s Rings

20 Image credit: NASA/JPL Ring Gap Moons

21 Image credit: Cassini ISS Ring Gap Moons

Daphnis/Keeler Gap Pan/Encke Gap

22 Image credit: Cassini ISS Ring Gap Moons

Daphnis/Keeler Gap Pan/Encke Gap

23 Image credit: Cassini ISS Beyond the solar system

… to other disks

24 Image credit: Cassini ISS HH objects: young stars and jets

New star forms, has “accretion disk” Jets of gas ejected by young star around it from collapsed cloud of gas/dust

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• Eventually, the violent environment of birth dissipates. • Disk of gas and dust remains • Dust starts to condense and grow…the seeds of planets!

26 Asteroid Belt

27 Spiral Galaxies

28 Black Hole Accretion Disks

29 Black Hole Accretion Disks

Credit: Kip Thorne

30 Questions?

31 Brief background and recent discoveries in the study of protoplanetary disks

Rachel Akeson

Image credit: ESO/L. Calçada – ESO 32 Formation of stars and planets: start

Credit: NASA/JPL: T. Greene

a. The star formation process starts in dense clouds of gas and dust. 1 AU (Astronomical Unit) = 93 million miles = distance from the Sun to the Earth b. The gravitational collapse only happens if the gas and dust are dense enough that the gravitational force overcomes the pressure force c. The central region is dense enough that nuclear fusion begins, it is called a protostar. The collapsing gas and dust forms a flat disk and more extended envelope. At the poles of the protostar, a bipolar outflow is formed due to conservation of angular momentum.

33 Formation of stars and planets - end

Credit: NASA/JPL: T. Greene

d. A is a young star with roughly solar mass. Most of the disk accretes onto the star, but the remaining material is called a protoplantery disk and may form planets. e. Stars are on the main sequence once they burn hydrogen in the core. Any remaining disk material and new dust formed by collisions within the planetary system form a debris disk. f. After the planets are completely formed, the material in the disk fully disperses and any debris disk comes from collisions.

34 Some of the current questions:

• What is the detailed structure of the dust and gas in the disk? • What happens if there is more than one star? • What determines how massive the star becomes? • When does planet formation start? • Which disks form planets and what determines the planet properties?

35 How do we see these disks?

(Sub-millimeter) IR = infrared near-IR = 10-4 cm mid-IR = 10-3 cm Optical and infrared sub-millimeter = 0.01 to 0.1 cm

Accretion onto star

Ultraviolet

Dust continuum = light emission from dust grains; depends on their size and temperature

Credit: Dullemond and Monnier. 2010 36 HST observations

In the optical and near-infrared, most of the light from the disks comes from scattered radiation off of small dust grains. This happens when light from the star hits a single dust grain and is re-directed. It can also change wavelength.

(dust continuum)

HST observations of the scattered radiation shows where the small dust grains are and what their properties are

Credit: NAOJ 37 The Challenge: The star can be 1000 to 100,000 times brighter than this scattered light

Solutions 1. Look at stars where the disk blocks the star 2. Use a coronagraph to block the star

Credit: SOHO

38 Edge-on disks

• These four T Tauri stars are all oriented such that the disk blocks the light from the central star. • All four stars are in the Taurus star formation region at a distance of ~140 and are a few million years old. • The images show the scattered light from the disk and in some cases (top row), from the outflow.

39 Modeling the disk

~500 AU Bright scattered light

Dark dust lane obscures central star Difference in brightness gives inclination

Credit: Chris Burrows (STScI) and the WFPC2 Science Team 40 HST with a coronagraph

• TW Hya is closer (~45 parsecs) than the stars in Taurus and is older, roughly ~10 million years old. • The disk is nearly face- on and shows structure in the small dust grains.

Credit:NASA / ESA / J. Debes, H. Jang-Condell, A. Weinberger, A. Roberge, G. Schneider, A. Feild 41 ALMA: Atacama Large Millimeter Array

• 66 radio telescopes located in the Atacama desert in Chile at an elevation of 5000 m. • Collaboration between Europe (ESO), North America (NRAO) and East Asia (NAOJ).

Credit: ALMA (ESO/NAOJ/NRAO) 42 Before ALMA

• HL Tau is a young star in Taurus. • Early interferometer observations revealed a circumstellar disk with a mass ~0.1 times that of our Sun.

Credit: Kwon et al 2015

43 With ALMA

HL Tau • The disk is the same total size as with the previous observations, but the high angular sensitivity of ALMA revealed a series of bright rings and gaps. 100 AU • The disk appears elongated because the system is viewed at an angle with respect to Earth, but is circular. • The gaps could be caused by forming planets, or changing dust properties within disk.

Credit: ALMA (ESO/NAOJ/NRAO) 44 And there’s more Credit: NASA/ESA TW Hya HST scattered light observations, image scaled to same size as ALMA Elias 2-27

Credit: S. Andrews (Harvard-Smithsonian CfA), ALMA (ESO/NAOJ/NRAO) 50 AU

• ALMA traces the large dust grains and shows several gaps within the HST/scattered light gap • The small grains extend much farther from the star than the large grains 45 Not just rings

Elias 2-27 • The disk around the young star Elias 2-27 shows a spiral structure, rather than rings. • These could be produced by either a large planet or star outside of the disk, or instabilities within the disk. • The is a collection of asteroids and dwarf planets in the Solar System orbiting 30 to 50 AU from the Sun.

Credit: L. Pérez (MPIfR), B. Saxton (NRAO/AUI/NSF), ALMA (ESO/NAOJ/NRAO), NASA/JPL Caltech/WISE Team 46 Coming soon: James Webb Space Telescope

Instruments: • MIRI: Mid Infrared Instrument • NIRCam: Near Infrared Camera (with a coronagraph) • NIRISS: Near-InfraRed Imager and Slitless Spectrograph • NIRSpec: Near Infrared Spectrograph

With 7 times the collecting area of Hubble, JWST will observe even fainter disks

47 Marc Kuchner (GSFC) 48 49 NASA’s Wide field Infrared Survey Explorer (WISE)

50 Our Kuiper Belt: An alien’s view.

60 microns

Kuchner & Stark 2010

51 Ooooo! Ahhhh!

52 Debris Disks: Homes of

Planet 9 AU from star 4-11 Jupiter masses

β Pictoris

53 NASA’s WISE mission saw 747 million sources.

Galaxies, asteroids, interstellar matter…

…and a few thousand debris disks/protoplanetary disks mixed in among them. 54 All WISE disk candidates must be inspected by eye in all available bands to remove galaxies, artifacts, asteroids, etc.

Debes et al. (2011), Kennedy & Wyatt (2013), Patel et al (2014), Padgett et al. in prep.

55 56 Try it now at DiskDetective.org!

278,121 subjects total to classify 2.6 million classifications done so far (60% complete) roughly 30,000 participants 57 Draw a Scientist Test 1983

David Wade Chambers 1983 58 Discovery: Peter Pan stars.

Disks that are around stars that you would think are too old to have disks.

59 WISE J080822.18-644357.3: The Oldest Known Pre-Transitional Disk around an M dwarf

Carina Association (45 MYr)

Oldest Disk-Hosting M dwarf known in a Young Moving Group

LIR/Lstar=0.08 -1 accreting 10-10 Msolar yr

Silverberg et al. (2016) Murphy et al. (2017)

60 Many transitional disks and debris disks are in “Moving Groups”, groups of stars born all at the same time in the same birth cloud.

These are all over the sky, so they are hard to find…unless you have 30,000 Disk Detective volunteers. 61 SUPERUSERS

Mid March, we start getting complaints that the site is malfunctioning.

“Marc: artman40 has reached 32000 classifications. He is having problems again, it seems that this happens when he is near the total of images uploaded.”

Turns out we have a group of very intense “superusers” who have EACH already classified ALL the subjects that are online.

62 ~22000 2172 Unregistered Number of Registered 50% of total users did 25% Disk Detective Users classifications of the total classifications 1416 1243 SUPERUSERS

Data as of 325 12/12/14 55 13 9

10.6 1-5 6-25 26-125 126-625 626-3125 3126-16K 16K-78K mean Number of Classifications 63 SUPERUSERS

Superusers made their own video tutorials for new users.

64 Thanks to Superusers, Disk Detective is now available in English, SUPERUSERS French, Spanish, German, Hungarian, Romanian, Russian, Japanese, Portuguese, Chinese (Simplified and Traditional) and Bahasa.

65 SUPERUSERS

With all our launch delays, our first follow-up observing proposal deadline snuck up on us.

So we asked the superusers for last minute help.

We taught the superusers how to research targets in VizieR and we selected 102 spring/northen hemisphere targets from 32,000 with help from superusers, via Google Spreadsheet and Google Forms.

Now this is part of our routine!

66 67 Superuser Hugo Durantini Luca from Cordobo, Argentina introduced us to the astronomers at the CASLEO observatory, and…

68 …drove 12 hours across South America to help out with an observing run!!

69 For Scientists

70 Draw a Scientist Test 2017

YOU

71 http://www.darkmatterday.com/

Next Universe of Learning Science Briefing: Thursday, October 5.

72 ASTC partnership

A Professional Development opportunity – How to Use NASA Resources; future funding resources available

• Seven webinars to be held in 2018, with these goals: • Increase knowledge of NASA Astrophysics-related concepts • Improve familiarity of NASA Astrophysics resources and ways to use them • Utilize real NASA data • Interact with NASA Subject Matter Experts • To participate in this webinar series, contact Wendy Hancock at [email protected] or Tim Rhue at [email protected] by December 31, 2017

As a follow-on to this webinar series, there will be an opportunity to apply for $2,500 mini-fund resources to be competitively awarded to selected institutions, in order to implement or facilitate programming, produce exhibits, etc., using Universe of Learning resources. 73 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. 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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