exoplanets - avcr.czsummer2016.asu.cas.cz/exoplanets_ondrejov2016.pdfbut where all the planets are?...
TRANSCRIPT
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Exoplanets
Ondřejov Summer School September 15, 2016
Petr Kabáth
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Observations of Venus
• Babylonian observations of Venus
span of more than 20 years
in approx. 17th century BC
• This copy from 7 BC in cuneiform
• Recognition of periodicity (Venus cycles)
• First recorded astronomical observations
• Ammisaduqa 4th after Hammurabi
British Museumhttp://www.britishmuseum.org/explore/highlights/highlight_objects/me/c/cuneiform_venus.aspx
V. G. Gurzadyan - http://arxiv.org/pdf/physics/0311035v1.pdf
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IAU Resolution: Definition of a "Planet" in the Solar System
Contemporary observations are changing our understanding of planetary systems, and it is important that our nomenclature for objects reflect our current understanding. This applies, in particular, to the designation "planets". The word "planet" originally described "wanderers" that were known only as moving lights in the sky. Recent discoveries lead us to create a new definition, which we can make using currently available scientific information.
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RESOLUTION 5A
The IAU therefore resolves that planets and other bodies in our Solar System, except satellites, be defined into three distinct categories in the following way:
(1) A "planet" [1] is a celestial body that (a) is in orbit around the Sun, (b) has sufficient mass for its self-gravity to overcome rigid body forces so that it assumes a hydrostatic equilibrium (nearly round) shape, and (c) has cleared the neighbourhood around its orbit.
(2) A "dwarf planet" is a celestial body that (a) is in orbit around the Sun, (b) has sufficient mass for its self-gravity to overcome rigid body forces so that it assumes a hydrostatic equilibrium (nearly round) shape [2], (c) has not cleared the neighbourhood around its orbit, and
(d) is not a satellite.
(3) All other objects [3], except satellites, orbiting the Sun shall be referred to collectively as "Small Solar-System Bodies".
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RESOLUTION 6A
The IAU further resolves:
Pluto is a "dwarf planet" by the above definition and is recognized as the prototype of a new category of trans-Neptunian objects.
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More schematic
http://www.iau.org/news/pressreleases/detail/iau0603/
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An Exoplanet
A planet orbiting a star other than Sun
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Extraterrestrial life – search for Earth-like planet Evolution of planetary systems Statistical distribution of planets in the Universe
Motivation for exoplanet search
Are we alone in the Universe Search for extraterrestrial life – Earth-like
planets Statistical distribution of exoplanets
How do planetary systems evolve?
Image NASA
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Outline
Dawn of exoplanets (modern era) What do we know now about exoplanets? What can we expect in the next decade?
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Jan Neruda
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http://web2.mlp.cz/koweb/00/03/37/00/56/pisne_kosmicke.pdf
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Otto Struve (1897-1963)
First thoughts how to
detect the alien worlds
- spectroscopy
- photometry
Paper from 1952 – On high
precision radial velocities measurements
http://articles.adsabs.harvard.edu/cgi-bin/nph-iarticle_query?1952Obs....72..199S&data_type=PDF_HIGH&whole_paper=YES&type=PRINTER&filetype=.pdf
McDonald Observatory archives
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Life in the Galaxy
Are we alone? Frank Drake - 1960
www.space.com
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N = R* x fp x ne x fl x fi x fc x L
N – number of civilizations able of radio comm. R* = the average rate of star formation in our galaxy
fp = the fraction of those stars that have planets
ne = the average number of planets that can potentially support life per star that has planets
fl = the fraction of planets that could support life that actually develop life at some point
fi = the fraction of planets with life that actually go on to develop intelligent life (civilizations)
fc = the fraction of civilizations that develop a technology that releases detectable signs of their existence into space
L = the length of time for which such civilizations release detectable signals into space
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So the answer was (in 1960)?
10-20
Carl Sagan - Cosmos
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But where all the planets are?
Since Struve's proposal of RV measurements
- no planets detected, yet There was instrumentation to detect planets in
1950s, so where are all the planets?
- a transit can be detected by 20cm telescope First Radial Velocity surveys targeting specific
stars
- solar type stars – because of assumption of possible life friendly environment
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And finally, first exoplanets detected
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Detection of extreme planets
A planetary system
around the millisecond
pulsar PSR1257 + 12
A. Wolszczan &
D. A. Frail
Letters to Nature
Nature 355, 145 - 147
(09 January 1992); http://www.nature.com/nature/journal/v355/n6356/abs/355145a0.html
Wikipedia
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http://chandra.harvard.edu/photo/2013/vela/
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http://www2.astro.psu.edu/users/alex/pulsar_planets_text.html
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http://science.nasa.gov/science-news/science-at-nasa/2006/05apr_pulsarplanets/
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But well, ….
Pulsars environments are the most hostile places for life
One of the main motivation is to find the extraterrestrial life, defined as we know it from the Earth (water, organic molcules, etc.)
Therefore, planets around solar type stars are more suitable targets for surveys
Solar type (spectral type similar F-K), Solar analogs (similar Teff), solar twins (same Teff, same metallicity)
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Radial Velocity surveys
Mesurements of Radial Velocities with high accuracies (m/s regimes)
Spectral type catalogs Serching among bright stars in the solar
neighbourhood First planet around solar type star detected by
radial velocity survey in 1995 So how does radial velocity measurement
work?
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Like for binaries just,
the mass of the object causing the radial velocity variation is much smaller
(planets are defined as less massive than 13 Jupiter Masses)
So, the accuracies needed are m/s instead of km/s as for bianaries
targeting suitable stars
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The Case of 51 Peg
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ELODIE at OHP
http://www.obs-hp.fr/www/guide/elodie/elodie-sans.html
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http://www.obs-hp.fr/www/guide/elodie/elodie-sans.html
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http://www.obs-hp.fr/www/guide/elodie/elodie-sans.html
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ELODIE
Echelle-spectrograph was located at Observatoire de Haute Provence at 1.93m telescope (now replaced by SOPHIE)
Permitted measurements with accuracy down to 15m/s for 9 mag stars
JUST A NOTE – WEATHER ABOUT 15 percent better than Ondrejov (ONLY)
http://articles.adsabs.harvard.edu/cgi-bin/nph-iarticle_query?1996A%26AS..119..373B&data_type=PDF_HIGH&whole_paper=YES&type=PRINTER&filetype=.pdf
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Mayor and Queloz,1995, Nature
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51 Peg Characteristics:
- detected 1995, Mayor and Queloz, Nature
- Mass: 0,45 M Jupiter
- Radius : 1,9 R Jupiter
- Period : 4.23 days
- Semi.-m.axis: 0.052 AU
- Star: G2 IV Mayor and Queloz, 1995, Nature, 378, 355
(http://www.nature.com/nature/journal/v378/n6555/abs/378355a0.html)
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RV surveys and planet types
After 51 Peg Radial velocity surveys begin to report new planets
Mostly they are so-called hot-Jupiters a new class of planets – close to the host, hot, Jupiter-sized, short orbital period
How did they get so close to the host star? What is the composition of their atmosphere? How common are they? And are there smaller planets too?
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51 Peg compared
Image from Keele University
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Exoplanets in 2000
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Can we detect a transit?
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Eclipses/transits
From Angerhausen et al. 2008
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Well, if we are lucky
NASA Kepler Space mission webpages
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Motivation to detect a transit?
Some planets should transit stellar discs (in line of sight towards the observer) especially the close-to-star ones
Geometrical probability of a transit of a hot-Jupiter is about 10 percent
Assuming every system with planet hosts a hot-Jupiter, then 1 in 10 should present a transit
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https://web.njit.edu/~gary/320/Lecture10.html
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When the planet eclipses its star
Charbonneau et al. 2000
HD209458b
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HD209458b Parameters
- Mass : 0.69Mj
- Radius : 1.38 Rj
- O. period : 3.5 days
Star: G0V
brightness: 7 mag (V)
Teff: 6092 K
Metallicity: 0.02http://mnras.oxfordjournals.org/content/418/3/1822
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Some statistics
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And are hot-Jupiters common? What is the occurance rate for hot-Jupiters?
- Fischer claims around 1 percent
- Jupiter sized planets at greater distances probably more common but difficult to detect (long orbital period)
Where are the small planets (Neptune - Earth)?
- undetected, high accuracy of cm/s needed but they seem to be very common
As of 2006
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Ground based transit survey projects
SuperWasp – the most successful ground based survey operated by UK universities
2 robotic observatories – La Palma, Spain and South Africa
Each site consists of 8 telescopes with wide angle CCDs
More than 100 planets discovered
since 2002
http://www.superwasp.org/index.html
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How many stars do have planets?(2006)
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New planets detected – small planets
GJ436b – Neptune-sized planet detected, first of its kind
Warm Neptune Mass: 0.07Mj Radius: 0.38 Rj Star: M2.5 SMALL PLANETS DO EXIST
BUTLER P., VOGT S., MARCY G., FISCHER D., WRIGHT J., HENRY G., LAUGHLIN G. & LISSAUER J.
ApJ. Letters, 617, 580
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OBSERVE AS MANY STAR AS POSSIBLE TO FIND TRANSITS
NASA web
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Detection methods
From: Perryman, Rep. Prog. Phys. 2000, 63, 1209 (updated May 2004)
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Space missions
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CoRoT
Convection, Rotation and planetary Transits
Launched 2006 – mission end 2013
28cm mirror, 4 detectors of 1,5x1,5deg
ESA webpages
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ESA webpages
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Kepler
1.4-m mirror, telescope equipped with an array of 42 CCDs, each of 50x25 mm CCD has 2200x1024 pixels.
launch March 2009, now continuing as K2
Monitored 100k stars in Cygnus constellation
Detected 1030 confirmed planets
More to come from K2
Kepler webpage - http://kepler.nasa.gov/
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Kepler
Determine the abundance of terrestrial and larger planets in or near the habitable zone of a wide variety of stars;
Determine the distribution of sizes and shapes of the orbits of these planets;
Estimate how many planets there are in multiple-star systems;
Determine the variety of orbit sizes and planet reflectivities, sizes, masses and densities of short-period giant planets;
Identify additional members of each discovered planetary system using other techniques; and
Determine the properties of those stars that harbor planetary systems.
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F Fressin et al. Nature 000, 1-5 (2011) doi:10.1038/nature10780
Transit light curves.
Note: This figure is from a near-final version AOP and may change prior to final publication in print/online
2 Earth like planets – Kepler 20 e and f
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http://kepler.nasa.gov/Mission/discoveries/
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How many planets do we know today? State of the art
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Plantes 2016
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Magnitude vs. radius
http://cheops.unibe.ch/science/corot-kepler-vs-cheops/
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Habitable zones (liquid water)
http://news.discovery.com/space/planetary-habitable-zones-defined-by-alien-biochemistry-111118.htm
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http://phl.upr.edu/projects/habitable-exoplanets-catalog
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And finally Prxoima Centauri b
ESO Press release http://www.eso.org/public/news/eso1629/
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What do we know about exoplanets?
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Characterization of exoplanets
https://www.spacetelescope.org/images/opo0707b/
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FORS2 2010, 2011
Bean et al. 2010, NatureBean, Desert, Kabath et al. 2011, AandA
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Weather on exoplanets
CHANGING PHASES OF ALIEN WORLDS: PROBING ATMOSPHERES OF KEPLER PLANETS WITH HIGH-PRECISION PHOTOMETRY
Lisa J. Esteves, Ernst J. W. De Mooij, and Ray Jayawardhana
The Astrophysical Journal, Volume 804, Number 2
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Weather on exoplanets (cont.)
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https://www.spacetelescope.org/news/heic1422/
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Finding life
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NGTS
http://www.ngtransits.org/survey.shtml
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NGTS
http://www.ngtransits.org/survey.shtml
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CHEOPS
32cm telescope
Launch 2017
http://sci.esa.int/cheops/54032-spacecraft/
http://cheops.unibe.ch/
Credit: ESA
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TESS
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Kaltenegger, L. and Traub, W. (2009) Transits of Earth-Like Planets. Astrophysical Journal
JWST Launch 2018Ideal for characterization of small planets in infraredImage NASA
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Plato Space mission
Credit: Thales Alenia Space
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PLATO Space mission
The instrument consists of 32 "normal" telescopes
Stars with mV > 8. Two additional “fast” cameras with high read-out cadence (2.5 s) will be used for stars with mV ~4–8
Each camera has an 1100 deg2 FoV and a pupil diameter of 120 mm and is equipped with a focal plane array of 4 CCDs each with 45102 pixels of 18 μm size
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E-ELT - 2024
EPICS – Exoplanet imagng camera and spectrograph
https://www.eso.org/sci/libraries/SPIE2010/7735-84.pdf
METIS - The Mid-infrared E-ELT Im. and Spectr. - 3–20 μm
Low-resolution (R < 1,000) at L,M,N
Medium-resolution (R <10,000) at N
High-resolution (R~100,000) IFU at L,M
HARMONI - is a visible and near-infrared (0.47 to 2.45 µm) integral field spectrograph, providing the E-ELT's core spectroscopic capability, over a range of resolving powers from R (≡λ/Δλ) ~500 to R~20000.
https://www.eso.org/public/images/ann15056a/
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E-ELT
Credit: ESO
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Artificial transiting structures
Arnold, 2005, ApJ
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Arnold, 2005, ApJ
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http://iopscience.iop.org/article/10.1088/0004-637X/809/2/139/pdf
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http://science.nasa.gov/science-news/science-at-nasa/2013/23jul_palebluedot/
THANK YOU
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PLATO Space missionPLAnetary Transits and Oscillations of stars
Theme: What are the conditions for planet formation and the emergence of life?
Primary Goal Detection and characterisation of terrestrial exoplanets around bright solar-type stars, with emphasis on planets orbiting in the habitable zone.
Photometric monitoring of a large number of bright stars for the detection of planetary transits and the determination of the planetary radii (around 2% accuracy)
Ground-based radial velocity follow-up observations for the determination of the planetary masses (around 10% accuracy)
Asteroseismology for the determination of stellar masses, radii, and ages (up to 10% of the main sequence lifetime)
Identification of bright targets fr spectroscopic follow-up observations of planetary atmospheres with other ground and space facilities
LAUNCH 2024
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JWST
MIRI - mid-IR camera
NIRI – near-IR camera
NIRSpec – near-IR spectrograph
NIRISS – near-IR imager and slitless spectrogr.
Exoplanets and Solar systém one of the key themes
Launch date 2018
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TESS
TESS is designed to:
Monitor 200,000 nearby stars for planets
Focus on Earth and Super-Earth size planets
Cover 400× larger sky area than Kepler
Span stellar spectral types of F5 to M5
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CHEOPS
The main science goals of the CHEOPS mission will be to study the structure of exoplanets with radii typically ranging from 1-6 REarth orbiting bright stars. With an accurate knowledge of masses and radii for an unprecedented sample of planets, CHEOPS will set new constraints on the structure and hence on the formation and evolution of planets in this mass range. In particular, CHEOPS will:
Determine the mass-radius relation in a planetary mass range for which only a handful of data exist and to a precision never before achieved.
Probe the atmosphere of known Hot Jupiters in order to study the physical mechanisms and efficiency of the energy transport from the dayside to the night side of the planet.
Provide unique targets for future ground- (e.g. E-ELT) and space-based (e.g. JWST, EChO) facilities with spectroscopic capabilities. With well-determined radii and masses, the CHEOPS planets will constitute the best target sample within the solar neighbourhood for such future studies.
Offer up to 10% of open time to the community to be allocated through competitive scientific review.
Identify planets with significant atmospheres as a function of their mass, distance to the star, and stellar parameters. The presence (or absence) of large gaseous envelopes bears directly on fundamental issues such as runaway gas accretion in the core accretion scenario or the loss of primordial H-He atmospheres.
Place constraints on possible planet migration paths followed during formation and evolution for planets where the clear presence of a massive gaseous envelope cannot be discerned.
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http://phl.upr.edu/press-releases/nasakeplerdiscoversnewpotentiallyhabitableexoplanets
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How did they form?
Evidence of the disk around pulsars (2006 Spitzer) Forming after the death of the star?
A debris disk around an isolated young neutron star
Zhongxiang Wang1, Deepto Chakrabarty1 & David L. Kaplan1
Nature 440, 772-775 (6 April 2006) | doi:10.1038/nature04669; Received 5 August 2005; Accepted 21 February 2006
Reading:http://science.nasa.gov/science-news/science-at-nasa/2006/05apr_pulsarplanets/
http://www.nature.com/nature/journal/v440/n7085/full/nature04669.html