Radial Velocity Detection of Planets:II. Results

• To date 701 planets have been detected with the RV method

• ca 500 planets discovered with the RV method. The others are from transit searches

• 94 are in Multiple Systems

→ exoplanets.org

Telescope Instrument Wavelength Reference

1-m MJUO Hercules Th-Ar

1.2-m Euler Telescope CORALIE Th-Ar

1.8-m BOAO BOES Iodine Cell

1.88-m Okayama Obs, HIDES Iodine Cell

1.88-m OHP SOPHIE Th-Ar

2-m TLS Coude Echelle Iodine Cell

2.2m ESO/MPI La Silla FEROS Th-Ar

2.7m McDonald Obs. Tull Spectroraph Iodine Cell

3-m Lick Observatory Hamilton Echelle Iodine Cell

3.8-m TNG SARG Iodine Cell

3.9-m AAT UCLES Iodine Cell

3.6-m ESO La Silla HARPS Th-Ar

8.2-m Subaru Telescope HDS Iodine Cell

8.2-m VLT UVES Iodine Cell

9-m Hobby-Eberly HRS Iodine Cell

10-m Keck HiRes Iodine Cell

Campbell & Walker: The Pioneers of RV Planet Searches

1980-1992 searched for planets around 26 solar-type stars. Even though they found evidence for planets, they were not 100% convinced. If they had looked at 100 stars they certainly would have found convincing evidence for exoplanets.

1988:

„Probable third body variation of 25 m s–1, 2.7 year period, superposed on a large velocity gradient“

Campbell, Walker, & Yang 1988

Eri was a „probable variable“

Filled circles are data taken at McDonald Observatory using the telluric lines at 6300 Ang as a wavelength reference

The first extrasolar planet around a normal star: HD 114762 with Msini = 11 MJ discovered by Latham et al. (1989)

51 Peg

Rate of Radial Velocity Planet Discoveries

51 Pegasi b: The Discovery that Shook up the Field

Discovered by Michel Mayor & Didier Queloz, 1995

Period = 4,3 Days

Semi-major axis = 0,05 AU (10 Stellar Radii!)

Mass ~ 0,45 MJupiter

Mass Distribution

Global Properties of Exoplanets:

i decreasing

probability decreasing

Because we only measure msini one could argue that all of these companions

are not planets but low mass stars viewed near i = 0 degrees.

P(i < ) = 1– cos Probability an orbit has an inclination less than

e.g. for m sin i = 0.5 MJup for this to have a true mass of 0.5 Msun sin i would have to be 0.01. This implies = 0.6 deg or P =0.00005: highly unlikely!

Argument against stars #1

This argument was probably valid when you had 10 exoplanets, but with 700 it is highly unlikely that all of them are stellar companions viewed at a low inclination

Argument against stars #2

We have detected approximately 200 transiting planets where we know the inclination. All of these have masses in the planetary regime.

The Brown Dwarf Desert

Mass Distribution

Global Properties of Exoplanets:

Planet: M < 13 MJup → no nuclear burning

Brown Dwarf: 13 MJup < M < ~80 MJup → deuterium burning

Star: M > ~80 MJup → Hydrogen burning

Brown Dwarf Desert: Although there are ~100-200 Brown dwarfs as isolated objects, and several in long period orbits, there is a paucity of brown dwarfs (M= 13–50 MJup) in short (P < few years) as companion to stars

An Oasis in the Brown Dwarf Desert: HD 137510 = HR 5740

The distinction between brown dwarfs and planets is vague. Until now the boundary was taken as ~ 13 MJup where deuterium burning is possible. But this is arbitrary as deuterium burning has little influence on the evolution of the brown dwarf compared to the planet

Brown Dwarfs versus Planets

Bump due to deuterium burning

A better boundary is to use the different distributions between stars and planets:

By this definition the boundary between planets and non-planets is 20 MJup

A note on the naming convention:

Name of the star: 16 Cyg

If it is a binary star add capital letter B, C, D

If it is a planet add small letter: b, c, d

55 CnC b : first planet to 55 CnC

55 CnC c: second planet to 55 CnC

16 Cyg B: fainter component to 16 Cyg binary system

16 Cyg Bb: Planet to 16 Cyg B

The IAU has yet to agree on a rule for the naming of extrasolar planets

Semi-Major Axis Distribution

The lack of long period planets is a selection effect since these take a long time to detect

The short period planets are also a selection effect: they are the easiest to find and now transiting surveys are geared to finding these.

Eccentricity versus Orbital Distance

Note that there are few highly eccentric orbits close into the star. This is due to tidal forces which circularizes the orbits quickly.

Eccentricity distribution

Fall off at high eccentricity may be partially due to an observing bias…

e=0.4 e=0.6 e=0.8

=0

=90

=180

…high eccentricity orbits are hard to detect!

For very eccentric orbits the value of the eccentricity is is often defined by one data point. If you miss the peak you can get the wrong mass!

2 ´´

Eri

Comparison of some eccentric orbit planets to our solar system

At opposition with Earth would be 1/5 diameter of full moon, 12x brighter than Venus

16 Cyg Bb was one of the first highly eccentric planets discovered

Mass versus Orbital Distance

There is a relative lack of massive close-in planets

Classes of planets: 51 Peg Planets: Jupiter mass planets in short period orbits

• ~40% of known extrasolar planets are 51 Peg planets with orbital periods of less than 20 d. This is a selection effect due to:

1. These are easier to find.

2. RV work has concentrated on transiting planets

• 0.5–1% of solar type stars have giant planets in short period orbits

• 5–10% of solar type stars have a giant planet (longer periods)

Classes of planets: 51 Peg Planets

Another short period giant planet

Butler et al. 2004

McArthur et al. 2004

Santos et al. 2004

Msini = 14-20 MEarth

Classes of planets: Hot Neptunes

Note that the scale on the y-axes is a factor of 100 smaller than the previous orbit showing a hot Jupiter

If there are „hot Jupiters“ and „hot Neptunes“ it makes sense that there are „hot Superearths“

Mass = 7.4 ME P = 0.85 d

CoRoT-7b

Hot Superearths were discovered by space-based transit searches

Classes of Planets: The Massive Eccentrics

• Masses between 7–20 MJupiter

• Eccentricities, e > 0.3

• Prototype: HD 114762 discovered in 1989!

m sini = 11 MJup

As of 2011 there were no massive planets in circular orbits

Classes: The Massive Eccentrics

Now there is more, but still relatively few. Ignoring the blue points (close in planets) there are ~ 10 planets with masses > 10 MJup with e < 0.2 and ~20 with e > 0.2

Classes: The Massive Eccentrics

Red: Planets with masses < 4 MJup

Blue: Planets with masses > 4 MJup

Planet-Planet Interactions

Initially you have two giant planets in circular orbits

These interact gravitationally. One is ejected and the remaining planet is in an eccentric orbit

Lin & Ida,  1997, Astrophysical Journal, 477, 781L

• Most stars are found in binary systems• Does binary star formation prevent planet

formation?

• Do planets in binaries have different characteristics?

• What role does the environment play?• Are there circumbinary planets? (see Kepler

Lecture!)

Why should we care about binary stars?

Classes: Planets in Binary Systems

Star a (AU)16 Cyg B 80055 CnC 540

HD 46375 300Boo 155 And 1540

HD 222582 4740HD 195019 3300

Some Planets in known Binary Systems:

There are very few planets in close binaries. The exception is Cep.

For more examples see Mugrauer & Neuhäuser 2009, Astronomy & Astrophysics, vol 494, 373 and references therein

If you look hard enough, many exoplanet host stars in fact have stelar companions

A new stellar companion to the planet hosting star HD 125612

Mugrauer & Neuhäuser 2009

Approximately 17% of the exoplanet hosting stars have stellar companions (Mugrauer & Neuhäuser 2009). Most of these are in wide systems.

The first extra-solar Planet may have been found by Walker et al.

in 1992 in abinary system:

Ca II is a measure of stellar activity (spots)

Cep Ab: A planet that challenges formation theories

2,13 AUa

0.2e

26.2 m/sK

1.76 MJupiterMsini

2.47 YearsPeriod

Planet

18.5 AUa

0,42 ± 0,04e

1.98 ± 0,08 km/sK

~ 0,4 ± 0,1 MSunMsini

56.8 ± 5 YearsPeriod

Binary Cephei

Cephei

Primary star (A)

Secondary Star (B)Planet (b)

Neuhäuser et al. Derive an orbital inclination of AB of 119 degrees. If the binary and planet orbit are in the same plane then the true mass of the planet is 1.8 MJup.

The planet around Cep is difficult to form and on the borderline of being impossible.

Standard planet formation theory: Giant planets form beyond the snowline where the solid core can form. Once the core is formed the protoplanet accretes gas. It then migrates inwards.

In binary systems the companion truncates the disk. In the case of Cep this disk is truncated just at the ice line. No ice line, no solid core, no giant planet to migrate inward. Cep can just be formed, a giant planet in a shorter period orbit would be problems for planet formation theory.

The interesting Case of 16 Cyg B

Effective Temperature: A=5760 K, B=5760 K

Surface gravity (log g): 4.28, 4.35

Log [Fe/H]: A= 0.06 ± 0.05, B=0.02 ± 0.04

16 Cyg B has 6 times less Lithium

These stars are identical and are „solar twins“. 16 Cyg B has a giant planet with 1.7 MJup in a 800 d period

Kozai Mechanism: One Explanation for the high eccentricty of 16 Cyg B

Two stars are in long period orbits around each other.

A planet is in a shorter period orbit around one star.

If the orbit of the planet is inclined, the outer planet can „pump up“ the eccentricity of the planet. Planets can go from circular to eccentric orbits.

This was first investigated by Kozai who showed that satellites in orbit around the Earth can have their orbital eccentricity changed by the gravitational influence of the Moon

Kozai Mechanism: changes the inclination and eccentricity

Planetary Systems: 94 Multiple Systems

The first:

Some Extrasolar Planetary Systems

Star P (d) MJsini a (AU) e

HD 82943 221 0.9 0.7 0.54 444 1.6 1.2 0.41

GL 876 30 0.6 0.1 0.27 61 2.0 0.2 0.10

47 UMa 1095 2.4 2.1 0.06 2594 0.8 3.7 0.00

HD 37124 153 0.9 0.5 0.20 550 1.0 2.5 0.4055 CnC 2.8 0.04 0.04 0.17 14.6 0.8 0.1 0.0 44.3 0.2 0.2 0.34 260 0.14 0.78 0.2 5300 4.3 6.0 0.16Ups And 4.6 0.7 0.06 0.01 241.2 2.1 0.8 0.28 1266 4.6 2.5 0.27HD 108874 395.4 1.36 1.05 0.07

1605.8 1.02 2.68 0.25HD 128311 448.6 2.18 1.1 0.25 919 3.21 1.76 0.17HD 217107 7.1 1.37 0.07 0.13 3150 2.1 4.3 0.55

Star P (d) MJsini a (AU) eHD 74156 51.6 1.5 0.3 0.65 2300 7.5 3.5 0.40

HD 169830 229 2.9 0.8 0.31 2102 4.0 3.6 0.33

HD 160691 9.5 0.04 0.09 0 637 1.7 1.5 0.31

2986 3.1 0.09 0.80

HD 12661 263 2.3 0.8 0.35

1444 1.6 2.6 0.20

HD 168443 58 7.6 0.3 0.53 1770 17.0 2.9 0.20HD 38529 14.31 0.8 0.1 0.28 2207 12.8 3.7 0.33HD 190360 17.1 0.06 0.13 0.01 2891 1.5 3.92 0.36HD 202206 255.9 17.4 0.83 0.44 1383.4 2.4 2.55 0.27HD 11964 37.8 0.11 0.23 0.15

1940 0.7 3.17 0.3

The 5-planet System around 55 CnC

5.77 MJ

Red lines: solar system plane orbits

•0.11 MJ ••

0.17MJ

0.03MJ

0.82MJ

The Planetary System around GJ 581

7.2 ME

5.5 ME

16 ME

Inner planet 1.9 ME

Can we find 4 planets in the RV data for GL 581?

1 = 0.317 cycles/d

2 = 0.186

3 = 0.077

4 = 0.015

Note: for Fourier analysis we deal with frequencies (1/P) and not periods

The Period04 solution:

P1 = 5.38 d, K = 12.7 m/s

P2 = 12.99 d, K = 3.2 m/s

P3 = 83.3 d, K = 2.7 m/s

P4 = 3.15, K = 1.05 m/s

P1 = 5.37 d, K = 12.5 m/s

P2 = 12.93 d, K = 2.63 m/s

P3 = 66.8 d, K = 2.7 m/s

P4 = 3.15, K = 1.85 m/s

=1.53 m/s=1.17 m/s

Almost:

Conclusions: 5.4 d and 12.9 d probably real, 66.8 d period is suspect, 3.15 d may be due to noise and needs confirmation.

A better solution is obtained with 1.4 d instead of 3.15 d, but this is above the Nyquist sampling frequency

Published solution:

Resonant Systems Systems

Star P (d) MJsini a (AU) e

HD 82943 221 0.9 0.7 0.54 444 1.6 1.2 0.41

GL 876 30 0.6 0.1 0.27 61 2.0 0.2 0.10

55 CnC 14.6 0.8 0.1 0.0 44.3 0.2 0.2 0.34

HD 108874 395.4 1.36 1.05 0.07 1605.8 1.02 2.68 0.25

HD 128311 448.6 2.18 1.1 0.25 919 3.21 1.76 0.17

2:1 → Inner planet makes two orbits for every one of the outer planet

→

→

2:1

2:1

→ 3:1

→ 4:1

→ 2:1

•

Eccentricities

Period (days)Red points: SystemsBlue points: single planets

EccentricitiesMass versus Orbital Distance

Red points: SystemsBlue points: single planets

Idea: If you divide the disk mass among several planets, they each have a smaller mass?

The Dependence of Planet Formation on Stellar Mass

2.9 2.0 1.6 1.2

RV

Err

or (

m/s

)

1.05 0.9 0.8 0.7 0.5

Stellar Mass (solar masses)

Main Sequence Stars

Ideal for 3m class tel. Too faint (8m class tel.). Poor precision

The shape of the previous histogram merely reflects the detection bias of the radial velocity method

Exoplanets around low mass stars (Mstar < 0.4 Msun)Programs:

• ESO UVES program (Kürster et al.): 40 stars• HET Program (Endl & Cochran) : 100 stars• Keck Program (Marcy et al.): 200 stars• HARPS Program (Mayor et al.):~200 stars

Results:

• ~15 planets around low mass (M = 0.15-0.4 Msun)

• Giant planets (2) around GJ 876. Giant planets around low mass M dwarfs seem rare• Hot neptunes around several → low mass start tend to have low mass planets

Currently too few planets around M dwarfs to make any real conclusions

GL 876 System

1.9 MJ

0.6 MJ

Inner planet 0.02 MJ

Exoplanets around massive stars

Difficult with the Doppler method because more massive stars have higher effective temperatures and thus few spectral lines. Plus they have high rotation rates. A way around this is to look for planets around giant stars. This will be covered in „Planets around evolved stars“

Result: Only a few planets around early-type, more massive stars, and these are mostly around F-type stars (~ 1.4 solar masses)

Galland et al. 2005

HD 33564

M* = 1.25

msini = 9.1 MJupiter

P = 388 days

e = 0.34

F6 V star

HD 8673

A Planet around an F star from the Tautenburg Program

Mplanet = 14.6 MJup Period = 4.47 Years ecc = 0.72

Frequency (c/d)

Sca

rgle

Pow

erP = 328 days

Msini = 8.5 Mjupiter

e = 0.24

An F4 V star from the Tautenburg Program

M* = 1.4 Mּס

Mstar ~ 1.4 Msun Mstar ~ 1 Msun

Mstar = 0.2-0.5 Msun

Preliminary conclusions: more massive stars have more massive planets with higher frequency. Less massive stars have less massive planets → planet formation is a sensitive function of the

planet mass.

Astronomer‘s

Metals

More Metals !

Even more Metals !!

Planets and the Properties of the Host Stars: The Star-Metallicity Connection

The „Bracket“ [Fe/H]

Take the abundance of heavy elements (Fe for instance)

Ratio it to the solar value

Take the logarithm

e.g. [Fe/H] = –1 → 1/10 the iron abundance of the sun

These are stars with metallicity [Fe/H] ~ +0.3 – +0.5

There is believed to be a connection between metallicity and planet formation. Stars with higher metalicity tend to have a higher frequency of planets. This is often used as evidence in favor of the core accretion theory

Valenti & Fischer

The Planet-Metallicity Connection?

There are several problems with this hypothesis

Endl et al. 2007: HD 155358 two planets and..

…[Fe/H] = –0.68. This certainly muddles the metallicity-planet connection

The Hyades

• Hyades stars have [Fe/H] = 0.2

• According to V&F relationship 10% of the stars should have giant planets,

The Hyades

• Paulson, Cochran & Hatzes surveyed 100 stars in the Hyades

• According to V&H relationship we should have found 10 planets

• We found zero planets!

Something is funny about the Hyades.

False Planets

or

How can you be sure that you have actually discovered a planet?

HD 166435

In 1996 Michel Mayor announced at a conference in Victoria, Canada, the discovery of a new „51 Peg“ planet in a 3.97 d. One problem…

HD 166435 shows the same period in in photometry, color, and activity indicators.

This is not a planet!

What can mimic a planet in Radial Velocity Variations?

1. Spots or stellar surface structure

2. Stellar Oscillations

3. Convection pattern on the surface of the star

Starspots can produce Radial Velocity Variations

Spectral Line distortions in an active star that is rotating rapidly

Rad

ial V

elo

city

(m

/s)

10

-10

0 0.2

0.4

0.6

0.8Rotation Phase

Tools for confirming planets: Photometry

Starspots are much cooler than the photosphere

Light Variations

Color Variations

Relatively easy to measure

Ca II H & K core emission is a measure of magnetic activity:

Active star

Inactive star

Tools for confirming planets: Ca II H&K

HD 166435

Ca II emission measurements

Bisectors can measure the line shapes and tell you about the nature of the RV variations:

What can change bisectors:• Spots• Pulsations • Convection pattern on star

Span

Curvature

Tools for confirming planets: Bisectors

Correlation of bisector span with radial velocity for HD 166435

Spots produce an „anti-correlation“ of Bisector Span versus RV variations:

Activity Effects: Convection

Hot rising cell

Cool sinking lane

•The integrated line profile is distorted.

•The ratio of dark lane to hot cell areas changes with the solar cycle

RV changes can be as large as 10 m/s with an 11 year period

This is a Jupiter!One has to worry even about the nature long period RV variations

The Planet around TW Hya?

Figueira et al. 2010, Astronomy and Astrophysics, 511, 55

A constant star

In the IR the radial velocity variations have 1/3 the amplitude in the optical. This is what expected from spots that have a smaller contrast in the IR

How do you know you have a planet?

1. Is the period of the radial velocity reasonable? Is it the expected rotation period? Can it arise from pulsations?

• E.g. 51 Peg had an expected rotation period of ~30 days. Stellar pulsations at 4 d for a solar type star was never found

2. Do you have Ca II data? Look for correlations with RV period.

3. Get photometry of your object

4. Measure line bisectors

5. And to be double sure, measure the RV in the infrared!

Radial Velocity Planets30 90 1000Period in years →

Red line: Current detection limits

Green line detection limit for a precision of 1 m/s

Summary Radial Velocity Method

Pros:

• Most successful detection method• Gives you a dynamical mass• Distance independent

• Will provide the bulk (~1000) discoveries in the next 10+ years

Summary

Radial Velocity Method

Cons:• Only effective for cool stars.

• Most effective for short (< 10 – 20 yrs) periods

• Only high mass planets (no Earths…yet!)

• Only get projected mass (msin i)

• Other phenomena (pulsations, spots, etc.) can mask as an RV signal. Must be careful in the interpretation

Summary of Exoplanet Properties from RV Studies

• ~5% of normal solar-type stars have giant planets

• ~10% or more of stars with masses ~1.5 Mּס have giant planets that tend to be more massive (more on this later in the course)

• < 1% of the M dwarfs stars (low mass) have giant planets, but may have a large population of neptune-mass planets

→ low mass stars have low mass planets, high mass stars have more planets of higher mass → planet formation may be a steep function of stellar mass

• 0.5–1% of solar type stars have short period giant plants

• Exoplanets have a wide range of orbital eccentricities (most are not in circular orbits)

• Massive planets tend to be in eccentric orbits and have large orbital radii

•Stars with higher metallicity tend to have a higher frequency of planets, but this needs confirmation