Lecture I: Hot Jupiter Discoveries

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Lecture I Hot Jupiter Discoveries

• Orbits and alignments
• Thermal properties
• The Mass-Radius diagram - interiors
• Tides and transit timing variations

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Lecture I Hot Jupiter Discoveries

• Orbits and alignments
• Thermal properties
• The Mass-Radius diagram - interiors
• Tides and transit timing variations

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Planets Orbiting Other Stars

• Total 209 discovered to-date.
• Statistics
• Gas giant planets, like Jupiter Saturn,
• exist around gt12 of stars (Marcy
  et al. 2005)
• Lower-mass planets (Super-Earths, 3 known
  to-date)
• are significantly more common
• (Rivera et al. 2005 Beaulieu et
  al. 2006).

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HD 209458b a Hot Jupiter
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HD 168443b highly eccentric one
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Hot Very Hot Jupiters
large Mp/Ms ratio small orbital
radius gtgt strong tides orbital decay

DS (2003) w updates
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Direct Detection of Thermal Emission
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Infrared Eclipses

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Infrared Eclipses in HD 189733 Measuring the
Emitted Heat
Time (in fraction of day)

Detection (Feb. 20, 2006) by Deming et al. using
the Spitzer Space Telescope
Relative Intensity or Brightness
Orbital phase
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Transit Measurements
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Properties of planets small stars
Models Baraffe et al. four different ages
0.5, 1, 3, 5 Gyr
Red Pont et al. (2005) OGLE-TR-122

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Transits Mass-Radius diagram
Transiting giant extra-solar planets - mean
densities
Bakos et al. (2006)
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Transits Mass-Radius diagram
All 14 known transiting giant extra-solar planets
Burrows et al. (2006)
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More diversity than expected ?...
Some of the Hot Jupiters do not match well models
based on Jupiter Saturn

Gaudi (2005) w Bodenheimer et al.(2003), Laughlin
et al. (2005) models Burrows et al. (2003
2006)
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More diversity than expected ?...
Some of the Hot Jupiters do not match well models
based on Jupiter Saturn

Charbonneau et al (2006) w Bodenheimer et
al.(2003), Laughlin et al. (2005) models and
Burrows et al. (2003 2006)
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The Measurement Errors

• In Mass
• What we derive is MP sini MS-2/3
• Transit phase helps in getting a good RV
  amplitude
• Know inclination, i, from transit light curve
• Use stellar models for MS - this is the
  dominant uncertainty.
• In Radius
• With one-band photometry - depends on MS and RS
• Good multi-band photometry - drop dependence on
  RS

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OGLE-TR-113b
P 1.43 days I 14.4 mag
Radial Velocities
Transit Light Curve
OGLE Udalski et al. (2003)
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Stellar Mass and Age
Stellar evolution track for 3 metallicities and
Helium content
Age 7 Gyrs
Stars evolve from bottom zero-age main sequence
Lines of constant stellar radii
HD 209458
Our Sun
Cody Sasselov (2002)
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HAT-P-1b the lightest
planet yet
RA 22 h 58 m Dec 38o 40 I 9.6 mag
G0 V Ms 1.12 MO Porb 4.46 days Mp 0.53
Mjup
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HAT-P-1 ADS 16402B
The HR diagram and evolutionary tracks fits
Bakos et al. (2006)
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The Measurement Errors

• In Mass
• What we derive is MP sini MS-2/3
• Transit phase helps in getting a good RV
  amplitude
• Know inclination, i, from transit light curve
• Use stellar models for MS - this is the
  dominant uncertainty.
• In Radius
• With one-band photometry - depends on MS and RS
• Good multi-band photometry - drop dependence on
  RS

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OGLE-TR-10b
P 3.10 days V 15.8 mag
Radial Velocities
Konacki, Torres, Sasselov, Jha (2005) green
brown points Bouchy, Pont, Melo, Santos, Mayor,
Queolz Udry (2004)
Transit Light Curve
OGLE Udalski et al. (2002)
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Improved photometry
Magellan telescope
Holman et al. (2005)
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Improved photometry
OGLE-TR-132b
VLT telescope
Moutou, Pont, Bouchy, Mayor (2004)
Original OGLE light curve
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Improved photometry
HD 209458b
Hubble Space Telescope - STIS
Wavelength- dependent limb darkening allows
more accurate RP and RS determination
Knutson et al. (2006)
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More diversity than expected ?...
Some of the Hot Jupiters do not match well models
based on Jupiter Saturn

Charbonneau et al (2006) w Bodenheimer et
al.(2003), Laughlin et al. (2005) models and
Burrows et al. (2003 2006)
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Comparison to theoretical models
What exactly do we compare?

Charbonneau et al (2006) w Bodenheimer et
al.(2003), Laughlin et al. (2005) models and
Burrows et al. (2003 2006)
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Interiors of Giant Planets

• Our own Solar System Jupiter Saturn
• Constraints M, R, age, J2, J4, J6
• EOS is complicated
• mixtures of molecules, atoms, and ions
• partially degenerate partially coupled.
• EOS Lab Experiments (on deuterium)
• Laser induced - LLNL-NOVA
• Gas gun (up to 0.8 Mbar only)
• Pulsed currents - Sandia Z-machine
• Converging explosively-driven - Russia (up to
  1.07 Mbar)

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Phase diagram (hydrogen)
Guillot (2005)
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Interiors of Giant Planets

• New hydrogen EOS Experiment
• Russian Converging explosively-driven system
  (CS)
• Boriskov et al. (2005)
• matches Gas gun Pulsed current (Z-machine)
  results
• deuterium is monatomic above 0.5 Mbar - no phase
  transition
• consistent with Density Functional Theory
  calculation (Desjarlais)

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Interiors of Giant Planets
Jupiters core mass and mass of heavy elements

For MZ - the heavy elements are mixed in
the H/He envelope
Saumon Guillot (2004)
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Interiors of Giant Planets
Saturns core mass and mass of heavy elements

Saumon Guillot (2004)
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Interiors of Giant Planets

• Core vs. No-Core
• How well is a core defined?
• Saturn metallic region can mimic core in J2
  fit (Guillot 1999)
• Core dredge-up - 20 MEarth in Jupiter, but MLT
  convection ?
• Overall Z enrichment
• Jupiter 7x solar
• Saturn 8x solar
• a high C/O ratio from Cassini ?

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Hot Jupiters Different Interiors ?...
Most Hot Jupiters will require large cores and Z
or/and Y enrichment

Gaudi (2005) w Bodenheimer et al.(2003), Laughlin
et al. (2005) models and Burrows et al. (2003)
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Interiors of Hot Jupiters

• Very wide range of radii
• small ones require cores enrichments larger
  than those of Jupiter and Saturn (Burrows et al.
  2006)
• large ones - their low densities are still
  difficult to explain
• additional sources of heat
• high-opacity atmospheres

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Interiors of Hot Jupiters
Hot Jupiters could capture high-Z planetesimals
if parked so close early

OGLE-TR-56b has Vorb 202 km/sec, Vesc 38
km/sec.
DS (2003) w updates
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Hot Jupiters Internal heating

• Tidal heating
• small ones require cores enrichments larger
  than those of Jupiter and Saturn (Burrows et al.
  2006)
• large ones - their low densities are still
  difficult to explain
• additional sources of heat
• high-opacity atmospheres

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Transit Timing Variations
Models of the HD 209458 system
Planet with P28.0 d
Planet with P19.2 d
Holman Murray (2005)
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The MOST Lightcurve of HD 209458
2005 observations, 40 minute binned data
0.03 mag
45 days

• 2004 data 14 days, 4 orbital cycles
• 2005 data 45 days, 12 orbital cycles
• duty cycle 90
• 473 896 observations
• 3 mmag point-to-point precision

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Transit Times 03, 04 05
Miller-Ricci MOST Team (2006)
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Transit Times 05
Miller-Ricci MOST Team (2006)
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Transit Times Results

• Second planet tidal scenario for the large Rpl
  of HD 209458b is entirely eliminated - excluded
  is any planet capable of causing its e gt 0.005
• No planets with M gt 0.6 ME in inner res (12)
• No planets with M gt 1 ME in outer res (21)
• No long-term Porb changes to level of 50ms
  over 3 years

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Challenges Spots Transits
MOST Team (2006) - Embargoed
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Interiors of Hot Jupiters

• Core vs. No-Core
• Core - leads to faster contraction at any age
• the case of OGLE-TR-132b gt high-Z and large
  core needed ?
• the star OGLE-TR-132 seems super-metal-rich
  (Moutou et al.)
• Cores nature vs. nurture ? - capturing
  planetesimals.
• Evaporation ? - before planet interior becomes
  degenerate
• enough - implications for Very Hot
  Jupiters
• the case of HD 209458b (Vidal-Madjar et al.
  2003) ?
• Overall Z enrichment
• After the initial 1 Gyr leads to more
  contraction.

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Summary Hot Jupiters

• Our gas giants - Jupiter Saturn
• have small cores
• are enriched in elements heavier than H (and He)
• The Hot Jupters we know
• most need cores enrichment
• four are on a diet or have secret affairs with
  another planet
• Is the core-accretion model in trouble ?
• not yet,
• but we should understand Jupiter and Saturn
  better.

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Issues

• Sizes of extrasolar planets are already precise
• but beware of biases systematic errors!
• Models are based on Jupiter Saturn
• Perhaps, Hot Very Hot Jupiters are more Z
  enriched
• because of history - excessive migration through
  disk, or
• because of orbit - manage to capture more
  planetesimals ?
• Implications for the core-accretion model
• it requires at least 6 ME for Mcore of Jupiter
  Saturn
• invoke Jupiter core erosion (e.g. Guillot 2005)
  ?

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Photometry of Extrasolar Planets

• Precise massive photometry
• OGLE Survey 5 transiting planets (10b, 56b,
  111b, 113b, 132b)
• TrES Survey 1 transiting planet (TrES-1)
• New parameters Radius Mean Density
• The Mass-Radius diagram
• Know inclination, hence Mass Radius are
  accurate
• Internal structure insights into planet
  formation.
• On-Off Photometry
• Atmospheric transmission in spectral lines
• Measurement of planets daytime IR thermal
  emission