Inte

ractions b

etw

een H

ot

Inte

ractions b

etw

een H

ot

Jupiters

Jupiters

and their H

ost S

tars

and their H

ost S

tars

Pin

Pin

-- Ga

oG

ao

Gu

Gu

AAc

ad

em

iac

ad

em

iaSS

inic

ain

ica

, ,

II ns

titu

te o

f n

sti

tute

of

AAs

tro

no

my &

s

tro

no

my &

AAs

tro

ph

ys

ics

,s

tro

ph

ys

ics

,

Ta

iwa

n

Ta

iwa

n

Typ

e o

f In

tera

cti

on

sT

yp

e o

f In

tera

cti

on

s

g

ravit

ati

on

al (t

ides in

ho

t Ju

pit

ers

& i

n h

ost

sta

rs)

m

ag

neti

c (

pla

net-

ind

uced

CaII

em

issio

ns;

pla

net

insid

e t

he A

lfven

rad

ius)

ste

llar

irra

dia

tio

n (

pla

neta

ry w

ind

s;

Ju

pit

er’

s s

ize)

33-- d

ay J

upit

er

Dese

rtd

ay J

upit

er

Dese

rt

tidal in

flation insta

bili

ty (

Gu, Lin

, &

Bodenheim

er

2003, 2004):

requires

critical eccentr

icitie

s, difficult for

massiv

e p

lanets

, lo

cation o

f dis

sip

ation

in

ner

dis

k tru

ncate

d b

y s

tella

r m

agnetic

field

s (

Lin

et al. 1

996):

wh

y 3

days? O

rby M

RI (K

uchner

& L

ecar

02):

handw

avin

g. O

r by e

vapora

tion

(Johnsto

ne)

R

oche-o

verf

low

driven b

y d

isk m

igra

tion

w/o

tid

al in

flation (

Trilli

ng e

t al. 1

998):

requires v

ery

larg

e p

lanet siz

es

o

rbit

al

deca

y d

ue t

o t

he s

pin

-orb

itti

dal in

tera

cti

on

(R

asio

et

al. 9

6;

Patz

old

& R

au

er

02;

Jia

ng

et

al. 0

2):

Q v

alu

e o

fa s

tar?

Meta

llic

ity

en

han

cem

en

t? F

aste

rste

llar

sp

in?

Wh

y i

s t

here

a p

ile-u

p?

orb

ital decay d

ue to m

agnetic inte

raction

(Shkoln

iket al. 2

005)

evapora

tion b

y s

tella

r irra

dia

tion/w

inds

(Vid

al-M

adja

ret al. 2

003):

sourc

e o

fneutr

al hydro

gen? M

agneto

sphere

of

a h

ot Jupiter?

Why p

ile-u

p?

c.f. bla

ck w

idow

puls

ar?

? 3-d

ay

Ju

pit

er

de

se

rt ? p

ile-u

p

of

ho

tJu

pit

ers

? p

au

cit

y

OG

LE

tran

sit

bia

s,

very

ho

tJu

pit

ers

bro

wn

dw

arf

de

se

rt

Dop

ple

r b

ias

cu

toff

peri

od

Q

sta

r~

10

5~

6(c

on

sis

ten

t w

ith

ste

llar

bin

ari

es)

fa

ste

r ro

tati

ng

sta

rs w

ith

hig

her

meta

llic

ity?

sta

rs h

avin

g v

ery

ho

t o

r m

assiv

e J

up

iters

rota

te f

aste

r?

ou

rJu

pit

er

OGLE Bias

OGLE Bias

2)

Po

nt

et

al. in

pre

para

tio

n

1)

Gau

di

et

al. 2

004

Rad

ial

Velo

cit

y S

urv

ey:

fixed

sam

ple

siz

ed

ete

cti

on

pro

bab

ilit

y3/

1)

sin

(−

∝P

iM

Kp

Tra

nsit

Su

rve

y:

fixed

S/N

dete

cti

on

pro

bab

ilit

y

3/5

13/

23

1)

)((

))(

(−

−−

−∝

∝P

PP

da

geom

etr

icS

/N# o

f sta

rs

RV

su

rve

y i

s c

on

sis

ten

t w

ith

Tra

nsit

su

rve

y

OG

LE

-TR

-111

neg

ati

ve c

orr

ela

tio

n

betw

een

[M

/H]

&V

sin

i:sp

in i

sn

’t d

ete

rmin

ed

b

y c

on

tam

inati

on

bu

t b

yco

nvecti

on

.

fast

rota

tor?

do

ub

le s

yn

ch

ron

ou

s? h

avin

g a

tra

ns

itin

g p

lan

et

at

0.0

31

AU

.

slo

w r

ota

tor

!V

sin

i<

5 k

m/s

(P

on

t et

al.)

co

nta

min

ate

d?

HD

377

Te

ff=

5872K

[M/H

]=0.1

1[F

e/H

]=0.1

5[S

i/H

]=0.0

5A

ge

iso=

2.7

1G

yr

Ag

ea

cti

vit

y=

0.2

4G

yr

Vsi

ni

vs

Vsi

ni

vs

[M/H

][M

/H]

(( Gu

Gu

, L

i,

, L

i, S

hko

lnik

Sh

koln

ik,

& L

iu 2

00

5,

& L

iu 2

00

5

bas

ed

on

bas

ed

on

Val

ent

iV

alent

i&

Fis

che

r 2

00

5)

& F

isch

er

20

05

)

Tw

o e

ffects

co

mp

ete

:ti

dal

sp

in-u

p (

Qs

tar)

mag

neti

c b

rak

ing

(K

w)

Spin Evo

lution

Spin Evo

lution

Ω=

−Ω

≈

×

Ω

≈

−−

=+

−=

ΩΩ

Ω

Ω

•

Ω

•

I

aGM

M

nRR

MMa

MMQ

RM

If

RR

MM

KR

M

I

star

p

tide

atide

star

sun

pJ

sun

star

sun

sun

sun

tide

star

sun

sun

star

wsun

sun

wind

magnetic

atide

magnetic

wind

tide

2

Gyrs

1/

1

AU

04

.0

10

1.0

15

.18

Gyrs

s/cm

g

10

7.2

days

3/2

1.0

19

.0

where

11

aa

11

1

,,

32

2/9

2/3

62

,

2/1

2/1

247

2

2

,,

τττ

πτ

ττ

ττ

τ

ke

y i

ssu

es:

m

ag

neti

c b

rakin

g (

theo

ry:

dyn

am

o &

win

d v

elo

cit

y,

ob

serv

ati

on

: S

ku

man

ich

rela

tio

nsh

ip P

rot∝ ∝∝∝

t1/2)

ti

dal d

issip

ati

on

: cir

cu

lari

zati

on

& s

yn

ch

ron

izati

on

wn

dp

ara

mete

r:cali

bra

ted

fo

r d

iffe

ren

t sp

ectr

al

typ

es

∝1/viscosity (for beginners),

constrained conventionally by binary stars

or by star-hot Jupiter systems?

PPro

tro

tevo

luti

on o

f evo

luti

on o

f ττ

Boo

B

oo ((

Gu

Gu

, L

i,

, L

i, S

hko

lnik

Sh

koln

ik,

& L

iu 2

00

5)

, &

Liu

20

05

)

win

d p

ara

mete

r: K

w=

0.4

Mp

= 5

MJ

Hard

to

dis

cri

min

ate

dif

fere

nt

Q-v

alu

es

Hard

to

sa

y τ τττ

Bo

ois

tid

all

y l

ocked

by i

tsp

lan

eta

ry c

om

pan

ion

un

less P

rot=

Po

rb

(wait

ing

fo

r M

OS

T r

esu

lts)

PPro

tro

te

volu

tion

of

evo

luti

on o

f O

GL

EO

GL

E-- T

RT

R-- 1

32

132

(( Gu

Gu

, L

i,

, L

i, S

hko

lnik

Sh

koln

ik,

& L

iu 2

00

5)

, &

Liu

20

05

)

Kw

= 6

.3 (

like K

-typ

e)

Mp

= 1

.01M

JQ

sta

r=

10

6

4 days

larg

e K

w

red

uc

e K

w

Q >

10

6

Q v

alu

e o

f a

so

lar-

typ

e s

tar

(Gu

, L

i, S

hko

lnik

, &

Liu

2005)

Can

Q=

10

6in

a s

tar

dri

ven

by a

ho

t Ju

pit

er

be r

ule

d o

ut?

Q=

10

6d

riven

by a

ste

llar

co

mp

an

ion

(M

ath

ieu

et

al.

2004);

need

an

oth

er

late

-F t

yp

e s

tar

to c

on

str

ain

th

e w

ind

para

mete

r K

wan

d t

hen

co

nstr

ain

th

e Q

valu

e o

fa s

ola

r-ty

pe s

tar.

Kw=

6.5

d

eri

ved

fro

m O

GL

E-T

R-1

32’s

cu

rren

t P

rot=

15 d

ays w

/o t

ides

Tidal Inf

lation

Tidal Inf

lation

(( G

uGu, , Bod

enh

eim

er

Bod

enh

eim

er , Lin 2

003, 2004)

, Lin 2

003, 2004)

tid

al

heati

ng

E

oS

evo

lves

therm

al

insta

bil

ity

run

aw

ay i

nfl

ati

on

R

och

e-l

ob

e o

ve

rflo

w

ou

tward

mig

rati

on

&m

ass l

oss

Ke

y W

ord

s:

Tid

al In

tera

ction

Poly

trope

Density I

oniz

ation

Ro

ch

e-l

ob

e o

ve

rflo

wth

res

ho

ld:

Qp=

10

6,

Mp=

1M

J,

Rp=

2R

J

un

ifo

rm h

ea

tin

g i

n m

as

s:

e≥0

.2 a

t a

=0

.04

AU

He

ati

ng

fo

cu

se

d o

n m

/Mp

=0

.9e≥0

.28

at

a=

0.0

4A

U

min

i in

tera

cti

ng

bin

ari

es

!

Most exoplanetsare eccentric(not due to observational bias!)

planet-disk interaction (Goldreich& Sari; Ogilvie& Lubow2003)

planet-planet interaction (Fort & Rasio)

0

0.1

0.2

0.3

0.4

0.5

0.6

0.7

0.8

0.91 0

.01

0.1

110

e

a (

AU

)

Tid

al

fric

tio

n,

bu

t b

ig e

wh

en

they a

re

yo

un

g

HD

80606b

Kozaim

echanis

m?

Cu

toff

peri

od

= 7

da

ys

tog

eth

er

wit

h

Ag

e 5

Gyrs

Q

valu

e

of

a J

up

iter

10

6

Gu

, B

od

en

heim

er,

& L

in 2

003

mass l

oss t

hru

L1

co

nstn

at

heati

ng

rate

p

er

un

it m

ass

no

in

ward

mig

rati

on

du

eto

dis

k-p

lan

et

inte

racti

on

fas

t in

fla

tio

nth

erm

al

ins

tab

ilit

y

Luminosity

Luminosity-- Radius Relation (

Radius Relation (Gu

Guet al. 2003, 2004)

et al. 2003, 2004)

2/3

9

25

10

6Degeneracy

rate)

cooling

( ,

/rate)

heating

(

TkT

E

RL

Qe

RH

Fermi

pp

p

−×

≅≡

∝∝

ρ

γ

Rp≈2

RJ

Rp≈2

RJ

γ>

5

therm

ally

sta

ble

γ<

5

therm

ally

unsta

ble

γ>

5

therm

ally

sta

ble

γ<

5

therm

ally

unsta

ble

Dege

nera

cy a

nd γ

decre

ases a

s R

p

incre

ases.

Polytrope

Polytropeand Planet Compressibility

and Planet Compressibility

(( Gu

Guet al. 2004)

et al. 2004)

effects.

ideal

-non

and

degeneracy

electron

of

reduction

the

to

due

increases

elasticity

splanet'

the

as decreases

modulus

bulk

adiabatic

the

i.e.

;

343

1 that

Note

.1

from

rises

as increases

and

entropy),

const.

at

size

(max

0 ,1

:degeneracy

partial

,0

,3/1

,0

:teroids

planets/as

lterrestria

3/1

5.1

const.,

:gas

degenerate

completely

31

lnln ,

3lnln

where

,ln

lnln

ln(entropy)

,

,

/3

1/1

1/1

1

M

ad

M

M

K

MK

KKpp

K

M

p

M

pK

Mp

n

p

n

pn

n

C

C

nC

Cn

CC

n

Cn

K

nn

Md

Rd

Cn

n

Kd

Rd

C

Md

CK

dC

Rd

Ks

RM

kK

KK

P

p

Γ

−

Γ=

≈≈

∞=

Γ=

==

−=

⇒=

=

−−=

≡

−=

≡

+=

⇒

∝=

≡=

+−

−+

Γρ

ρ

Form

ation o

f H

ot

Neptu

ne in 5

5 C

nc

(pre

limin

ary

)P

rog

en

ito

r m

igh

t b

e a

ho

t Ju

pit

er.

inte

rmit

ten

t m

ass l

oss d

ue t

oti

de +

secu

lar

pert

urb

ati

on

Rro

che/R

Ju

pite

r

Rp/R

Jup

ite

r

0.1

04

0.1

06

0.1

08

0.1

1

0.1

12

0.1

14

0.1

16

0.1

18

0.1

2

0.1

22 0

.4 0

.40

02

0.4

00

4 0

.40

06

0.4

00

8 0

.40

1

e

t (M

yr)

Secu

lar

reso

nan

ce s

ho

uld

be i

nclu

ded

(Nag

asaw

a&

Lin

2005)

CaII

CaII

from

Hot Jupiter

Host S

tars

from

Hot Jupiter

Host S

tars

CF

HT

VL

T

Hot Jupiters

Sh

ko

lnik

, W

alk

er,

Bo

hle

nd

er,

Gu

, &

Ku

rste

r200

5

CF

HT

: 2001 A

ug

(3.5

nig

hts

), 2

002 J

uly

(4

nig

hts

), 2

002 A

ug

(2 n

igh

ts)

2003 S

ep

(5 n

igh

ts)

VL

T:

2004 A

pr

(4x0.5

nig

hts

)

Pla

net

Mass &

P

lanet

Mass &

CaII

CaII

variation

variation

Sh

ko

lnik

, W

alk

er,

Bo

hle

nd

er,

Gu

, &

Ku

rste

r200

5

nig

ht-

to-n

igh

tC

aII

va

riati

on

τB

oo

:clo

se t

od

ou

ble

syn

ch

ron

ou

s

sta

te

mag

neti

c m

om

en

tin

cre

ase

s w

ith

pla

net

mass

in t

he S

ola

r S

yste

m (

Arg

ee

t al.

95)

M

ag

neti

c i

nte

racit

on

?

Synchro

niz

ed P

lanet

Synchro

niz

ed P

lanet --

induced H

eating?

induced H

eating?

Sh

ko

lnik

, W

alk

er,

Bo

hle

nd

er,

Gu

, &

Ku

rste

r200

5

2001 A

ug

(cir

cle

), 2

002 J

uly

(sq

uare

), 2

002 A

ug

(tr

ian

gle

), 2

003

Sep

(d

iam

on

d)

Pro

t=7

da

ys

Po

rb=

3.0

92

da

ys

Pro

t=1

4d

ays

Po

rb=

4.6

18

da

ys

du

e t

oste

llar

cycle

?m

ore

acti

ve

sm

all

er

co

ron

a h

ole

lo

ng

er

heati

ng

ph

ase

=10

27

erg

/s(1

.5x10

5erg

/cm

2s)

co

mp

ara

ble

to

a s

ola

r fl

are

win

din

g f

ield

lin

es

ph

ase d

iffe

ren

ce

Planet

Planet-- Induced

Induced Chromospheric

Chromospheric(( CaII

CaIIH & K emission) Activity

H & K emission) Activity

(( Shkolnik

Shkolnik, Walker,

, Walker, Bohlender

Bohlender, , Gu

Gu, &

, & Kuerster

Kuerster 2005)

2005)

Mag

neti

c H

eati

ng

?S

hane

Ern

o’s

con

cep

tion

of

the

fla

re

τ τττBoo

Boo

Boo

Boo

HD179979

for

G

10

G,

250

fields)

(dipole

3 ,

fields)

(open

2

if

s cm

erg

10

22

8

)/

)()(

8/(

*

12

5

2

*

)/1

1(2

*

/2

)/1

1(2 *

2

*,

2

≈≈

⇒

==

≥

−

=

−

−−

−−

p

p

qp

rot

orb

q

p

q

mwind

orb

m

BB

qp

RR

aR

PP

aB

B

Rr

VV

B

ππ

π

πφ

ho

t Ju

pit

er

insid

e t

he A

lfve

nra

diu

s

1)

no

sh

ock c

au

sed

by s

tell

ar

win

ds

(Zark

aet

al.

2001,

Ipet

al.

2004)

2)

Alf

ven

wave p

acket

tra

vel

inw

ard

ag

ain

st

ste

llar

win

ds

req

uir

es v

ery

larg

e s

tell

ar

field

s +

Alf

ve

nw

ave

s r

efl

ect

back f

rom

th

e s

tar

En

erg

y B

ud

ge

t P

rob

lem

?

Tri

gg

ere

d E

ne

rgy R

ele

as

e(G

u,

Li,

Sh

ko

lnik

, &

Liu

20

05

)

sam

e m

ag

nit

ud

eo

f a t

yp

ical

so

lar

flare

Int

rigu

ing

corr

ela

tion

for

th

e t

rans

itin

g pl

ane

tsInt

rigu

ing

corr

ela

tion

for

th

e t

rans

itin

g pl

ane

tsM

azeh

, Z

ucker,

& P

on

t 2005

evap

ora

tio

n in

sta

bil

ity

if M

p<

Mc

rit,

t eva

po

rati

on<

t KH

need

reli

ab

le

evap

ora

tio

n m

od

els

;n

o c

orr

ela

tio

n w

ith

L*

Ω ΩΩΩ*-

nti

dal in

tera

cti

on

larg

er

Mp

faste

ro

rbit

al d

ecay

bu

t vsin

i<5 k

m/s

fo

r O

GL

E

mag

neti

c i

nte

racti

on

larg

er

Mp

str

on

ger

B?

bu

t vsin

i<5 k

m/s

fo

r O

GL

EE

nerg

y b

ud

get

pro

ble

mR

och

e-l

ob

e o

ve

rflo

wo

verf

low

re

du

ce

Mp

& m

igra

te o

utw

ard

line

ar

rela

tion (

transit)

+ 3

-da

y J

up

iter

desert

(R

V)

.......

same

&

If

3/10

*

*

3/13

tP

Q

tM

QP

p

−∝

−∝

Sum

mary

Sum

mary

G

ravit

ati

on

al

Inte

racti

on

: ti

des i

n h

ost

sta

rs:

ste

llar

mo

dels

w/o

co

nsid

eri

ng

th

e t

idal

eff

ect

see

m t

o s

uff

icie

ntl

y e

xp

lain

Vsin

i/P

rot

T

he t

idal

dis

sip

ati

on

para

mete

r Q

in a

so

lar-

typ

e s

tar

dri

ven

by a

h

ot

(very

ho

t) J

up

iter

mig

ht

be m

uch

larg

er

than

th

at

dri

ven

by a

ste

llar

co

mp

an

ion

wit

h lo

ng

er

orb

ital

peri

od

sti

des i

n a

yo

un

g J

up

iter:

tid

al in

flati

on

in

sta

bilit

y

1)

a p

ile o

f

ho

t Ju

pit

ers

aro

un

d 0

.04-0

.05 A

U

2)

mass

-peri

od

rela

tio

n

for

ve

ry h

ot

Ju

pit

ers

3)

form

ati

on

of

ho

t N

ep

tun

es

4)

90%

of

ho

t Ju

pit

ers

mig

ht

ha

ve p

eri

sh

ed

(I

da &

Lin

04)

M

ag

neti

c I

nte

racti

on

:

Ob

serv

ati

on

: C

aII

em

issio

ns f

rom

HD

179

949 a

nd

υ υυυA

nd

are

s

yn

ch

ron

ized

wit

h p

lan

et’

s o

rbit

al

mo

tio

n,

bu

t th

ere

are

p

hase d

iffe

ren

ces.

Th

e e

nerg

y r

ele

as

e i

s c

om

para

ble

to

a

typ

ical

so

lar

flare

.P

ossib

le s

cen

ari

o:

Inw

ard

tra

veli

ng

Alf

ve

nw

ave

s a

lon

g

win

din

g f

ield

lin

es t

rig

ger

the m

ag

neti

c e

nerg

y a

lread

y

sto

red

on

th

e s

urf

ace o

f th

e h

ost

sta

r.