gu inica gao s s interactions between hot jupitersand...
TRANSCRIPT
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.