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Transcript of like this
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like this
FIELD BLUE STRAGGLERS AND
RELATED MASS TRANSFER ISSUES
George Preston, ESO, Santiago, 2012
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or this
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We stand on the shoulders of giants who pioneered stellar structure and evolution in interacting binaries
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my giants
G. P. Kuiper
O. StruveZ. Kopal
R. Kippenhahn
B. Paczynski
F. Hoyle
H. Bondi
W. H. McCrea
L. Lucy
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my giants
G. P. Kuiper
O. StruveZ. Kopal
R. Kippenhahn
B. Paczynski
F. Hoyle
H. Bondi
W. H. McCrea
L. Lucy
mentor
mentor
friendfriend
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G. P. Kuiper
O. StruveZ. Kopal
R. Kippenhahn
B. Paczynski
F. Hoyle
H. Bondi
W. H. McCrea
DetachedSemi-detached
Contact
gas streamsBeta Lyrae
Bondi-Hoyle accretion
Hoyle-Bondi accretion
The BS mass-transfer
model
CasesAB&C
Roche lobe overflow
Mass transfer
The Algol paradox
& more L. Lucy
The mostcamera-shy
giant known
my giants
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M3
M3, where it all started
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In a dense stellar environment
Allan Sandage PhD thesis
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unlike my FBS domain
.
.
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mostlyempty space
.
.
and here
like here
etc.
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While reading papers on the subject of my talk, I was surprised to learn …
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how often first-class astronomers ignore each other’s work!
Thus,Sandage (AJ 1953) first identified blue stragglers unambiguosly in M3
McCrea invented an explanation for Sandage’s blue stragglers 11 years later (MNRAS 1964) with no reference to Sandage.
Böhm-Vitense (ApJ 1980) confirmed operation of McCrea’s process 16 years later in the ζ Capricorni system with no reference to eitherSandage or McCrea.
McClure (ApJ 1984) brilliantly generalized Böhm-Vitense’s result 4 years later with no reference to Sandage or McCrea or Böhm-Vitense.
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how often first-class astronomers ignore each other’s work!
Thus,Sandage (AJ 1953) first identified blue stragglers unambiguosly in M3
McCrea invented an explanation for Sandage’s blue stragglers 11 years later (MNRAS 1964) with no reference to Sandage.
Böhm-Vitense (ApJ 1980) confirmed operation of McCrea’s process 16 years later in the ζ Capricorni system with no reference to Sandage or McCrea.
McClure (ApJ 1984) brilliantly generalized Böhm-Vitense’s result 4 years later with no reference to Sandage or McCrea or Böhm-Vitense.
Three decades of ignoring!
WTF!
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Finally, in 1989 Peter Leonard set the stage for this conferenceAJ 98, 217
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HOW TO IDENTIFY FBS
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Of necessity, in the field we first identified metal-poor FBS by colorimetry.
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Preston et al. 1994
BM
P st
ars
HK Survey: Beers et al. 1985, 1992
MS [Fe/H] = 0
MS [Fe/H = 1
Metal poor stars near GC turnoff
BHB
W. W. Morgan would have calledthe BMP stars a“natural group”.
Of necessity, in the field we first identified metal-poor FBS by colorimetry.
Any photometricsystem with a
uv filter will work.
RHB
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Preston et al. 1994
BM
P st
ars
HK Survey: Beers et al. 1985, 1992
MS [Fe/H] = 0
MS [Fe/H = 1
Metal poor stars near GC turnoff
BHB
W. W. Morgan would have calledthe BMP stars a“natural group”.
Of necessity, in the field we first identified metal-poor FBS by colorimetry.
Any photometricsystem with a
uv filter will work.
RHB
FBS area subset of BMP
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In BMP domain isochrones with a wide range
of ages and metallicities overlap in a tangled mess.
Preston & Sneden 2000
Isochrones of various [Fe/H] values and ages overlap in a 2-color diagram of the BS domain.
RYI IsochronesGreen et al. (1987)
main sequence isochrones
subgiant isochrones
Turnoffs for: [Fe/H] = 2.2 ages 3 7,10 Gy
Hence, “straggle”
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The cool (red) edge of the BS domain in any stellar system is defined by stars
that are not members of the domain
STRANGE DEFINITION
Mandushev, Fahlman, Richer 1997, AJ
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MOST FBS ARE A SUBSET OF A LARGER FAMILY OF MAIN SEQUENCE MASS TRANSFER BINARIES
Mandushev, Fahlman, Richer 1997, AJ
Use of MSTO coloras a boundary
obscures this reality
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12 Gy isochrone
surely FBS
CS 22949-008pri. & sec.
CASE IN POINTMetal-poor carbon stars below MSTO in hierarchical triples
Masseron et al. 2012, ApJ, 751:14
mass transfer sequence
CS 22964-161
= CEMP, literature
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Various tools have been devised to isolate field blue stragglers.Pier (1983) pioneered the identification of FBSs.
FBS
BHBD(0.2)
0.2
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Various tools have been devised to isolate field blue stragglers.Sersic (b,c) Balmer parameters do this particularly well.
They do not require knowledge of photometric colors.
FBS
BHB
Clewley et al. 2002
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Various tools have been devised to isolate field blue stragglers.Sersic (b,c) Balmer parameters do this particularly well.
They do not require knowledge of photometric colors.
FBS
BHB
Clewley et al. 2002
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An application of Sersic parameters to Sloan data in the distant halo
(n = 4985)
(n = many)
Xue et al. 2011
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Sarajedini 1993, ASP Conf. Ser.
Globular clusters provide luminosity calibrationfor Galactic structure applications, e.g. halo (R)
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MV) ~ 0.5 mag/star(distance) ~ 3 %/100 stars
Sarajedini 1993, ASP Conf. Ser.
Globular clusters provide luminosity calibrationfor Galactic structure applications, e.g. halo (R)
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GROUP PROPERTIES OF FBS
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It is easy to find binaries among FBS candidates
RV-constant stars Binary stars
A child can do it.
JD - 2400000
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A high % of FBS are members of spectroscopic binaries
Preston & Sneden 2000
4 km/s
20 km/s
vertical scales are not uniform
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Very high
Preston & Sneden 2000, AJ
A high % of FBS are members of spectroscopic binaries
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But a low % of FBS are in double-lined spectroscopic binaries
Very low
≤
The one DLSB, CS 22873-139, included here is contested by Spite et al. 2000, A&A, 360, 1077
Preston & Sneden 2000, AJ
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FBS have longish orbital periods & a high % of small orbital eccentricities reminiscent of their carbon-star cousins
deficit of short periods excess of low
eccentricitiesat P > 100 d
Normal MS binaries disk = xhalo = o
BMPblue metal-poor
C, s-process rich
Preston & Sneden 2000, AJ
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and their mass functions suggest companions of lower-than-normal mass (like maybe white dwarfs?).
f1 = K13 P / (2 π G) = M2
3 (sin3 i) / (M1 + M2)2
FBS Ba, CH cousins
Preston & Sneden 2000, AJ
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All of the preceding:High binary fractionDeficit of short periodsLow orbital eccentricitiesSmall mass functionsNo visible secondaries *And Thank You, Erika, for Capricorni
tell us that FBS are a species sui generis
* Hierarchical triples excepted
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white dwarfflux red wing of L
in white dwarf
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All of the preceding:High binary fractionDeficit of short periodsLow orbital eccentricitiesSmall mass functionsFew (no?) visible secondariesAnd Thank You, Erika, for Capricorni
tell us that FBS are a species sui generis
My perspective:Wide binary disruption is main reason
for the specific frequency deficitIn GCs relative to the Galactic field
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4.0
FBS
FBS
Specific frequency of FBS appears to be the upper bound of a sequence defined by OCs (DeMarchi et al 2006) and GCs (Piotto et al 2004)
This is a lo
garithm
This isn’t
Something like “concentration” must be what matters
Preston & Sneden 2000, AJ
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visualbinaries
c.p.m.binaries{
radial velocitybinaries P<4000 d
This 13% of radial velocity binaries with P 5 d merge in less than a Hubble time (Vilhu, 1982, A&A, 109, 17). Hence, the deficit of short period binaries in the field.
These more frequent wide binaries are largely disrupted in GCs. Hence, the relatively low specific frequency of blue stragglers in globular clusters.
This interpretation follows fromthe presumption that the
Duquennoy-Mayor (1991, A&A)period distribution is universal.
Ockham’s Razor, etc
William of Ockham1248-1307
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DUSTING
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How do you hide it?
DUST: A thin layer that you notice on tables
just before your guests arrive
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In the house use this
DUST: A thin layer that you notice on tables
just before your guests arrive
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In stars redistribute by thermohaline mixing.
DUST: A thin layer that you notice on tables
just before your guests arrive
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Reconciliation of theory and observation
Observational facts/issues that can be improved:
Numbers, orbital parameters of MS and post-MS C and Ba starsDetection criteriaDetection threshholds, bias, completenessObserver persistence (RV)
Theory:
Mass transfer by winds Including stuff like Davies-Pringle (1980) paradox
AGB theory and practice from Busso & Gallino andConvective envelopesGravitational settling and stabilizing molecular gradientsDilution with and without thermohaline mixing
those
those
all
other Italians
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those
all
Do all MS CEMP survive the RGB ascent?
INNOCENT QUESTION:
Is the observed density ratio (RGB)/(MS) OK?
MS CEMP(RGB)
CEMP(MS)
(kpc-3) = space densityn = nuclear time scale
relative volumes searched (in apparent magnitude limited surveys)
RGB
IF LRGB /LMS ~ 40
Volume ratio ~ 250 andn(RGB)/n(MS) ~ 102
THENVol* n ~ 2.5
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those
those
all
Stars with “no-dilution” solutions
dilution = log MCE/MAGBacc
x
dilutions from Bisterzo et al. 2012, MNRAS, 422, 849
All the stars with “no-dilution” solutionslie near MSTO; ~ half are FBS)
MSTO
RGB(CEMP)/MS(CEMP) ~ 2.5 in Bisterzo et al. sample. I was a bit surprised.
dilu
tio
n
pure AGB
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We have very little information about wind accretion at large distances from an AGB donor.
[s]
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Regression below is anchored by two long-period SLSBswith primaries originally classified as ordinary GK giants!
Griffin 1985
G8 III
K0 III
[s]
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Regression below is anchored by two long-period SLSBswith primaries originally classified as ordinary GK giants!
Griffin 1985
G8 III
K0 III
Want more candidates? See McWilliam 1990, ApJS, 74
23/671= 4% of GK giantsV(mag) 6.0, [s] > 0.2 Expect 800 more in HD (V<11)
[s]
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A bunch of calculations for MS stars with various
ages and [Fe/H]
Pinsonneault, DePoy, & Coffee 2001, ApJ
FBS convection zone rapidly disappears at Teff > 6500 K
He, Sr, Ba, sink in M2 prior to AGB evolution of M1.
Negative –gradient inhibits thermohaline mixingWhat happens when Ba-rich long-P FBS ascends RGB?
Will we recognize it, or will it disappear?
7000
-3.5
-4.0
Humoris still alive in
the USA!
FBS live here
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Jorissen & Van Eck 2001
F-G binaries ofDuquennoy & Mayor 1991
VB
CPM
The period distribution of Ba stars declines at P > 2000 d and dies at P ~ 5000 d, but the period distribution of MS binaries peaks at P > 10000 d.
Extant data provide a clue.
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Jorissen & Van Eck 2001
F-G binaries ofDuquennoy & Mayor 1991
VB
CPM
The period distribution of Ba stars declines at P > 2000 d and dies at P ~ 5000 d, but the period distribution of MS binaries peaks at P > 10000 d.
Extant data provide a clue.
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Orbital speeds at P = 10000 days are easily measured by modern spectrographs.
An unavoidable conclusion: winds “run out of gas” at some long P. Which?
2 3 4 5 6
log P(days)
0
5
10
15
20
K1 (k
m/s
)
m1 = 0.8, m2=0.5
K13P = constant
Newton’s laws are very tolerant of long orbital periods.
VB CPMRV
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THOSE YOUNG A-TYPE STARS ABOVE THE PLANE:
ANOTHER INCONVENIENT TRUTH
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This all began with Perry and Rogers, Harding & Sadler
Perry 1969 Rogers, Harding & Sadler 1981
I circled and boxeddata for
metal-rich A starsthat stray far from
Galactic plane
AVG = 5250 AVG = -0.23
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This all began with Perry and Rogers, Harding & Sadler
Perry 1969 Rogers, Harding & Sadler 1981
I circled and boxeddata for
metal-rich A starsthat stray far from
Galactic plane
AVG = 5250 AVG = -0.23
Santos et al. 2009, A&AThe average [Fe/H] for these A-Stars 5 kpc from the Galactic plane is only slightly lower than average value near the sun.
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Density distributions of early A-type stars far from the Galactic planehave a two-slope signature
Perry 1969 Lance 1988
north south
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Perry 1969 Lance 1988
The Lance (1988) stars below the Galactic plane are hotter than the BMP stars studied by Preston & Sneden (2000).
north south
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Perry 1969 Lance 1988
isochrone fort = 5.0E+8 y
They are apparently quite youngIf they are blue stragglers, what do they straggle behind?
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Perry 1969 Lance 1988
isochrone fort = 5.0E+8 y
They are apparently quite youngIf they are blue stragglers, what do they straggle behind?
Lance hypothesis: star formation during recent interaction
of a metal-poor, gas-rich satellite with the disk of the Milky Way.
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CHEMICAL ABUNDANCES ABOVE AND BELOW
THE MSTO
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Deep mixing accompanying merger, collision, mass transferburns 7Li to 4He ash low Li is a straggler signature.
BUT confirmation requires a big telescope for most FBS.
Data from Thorburn 1994, ApJ, 421
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data from P&S 2000, AJ
Galactic FBS
dSph red giants
halo stars
Compare dSph red giants to Galactic stars – Venn et al. 2004, AJ
thick disk
thin disk
What we might learn from the -elements.
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What we might learn from the -elements.
data from P&S 2000, AJ
Galactic FBS
dSph red giants
halo stars
Compare dSph red giants to Galactic stars – Venn et al. 2004, AJthick disk
thin disk
RV-constant BMP stars: Intermediate-Age captures
from a dSph satellite like Carina?
Stetson et al. 2011, ESO Messenger
13 Gy
8 Gy
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CH
The “non-variable” spectrum is the
mean of three stars
The FBS binary CS 29497-030 illustrates how the carbon signature responds to an increase in Teff
C I
Enter the AGB: Carbon and n-capture elements
G-band becomes inconspicuous
Atomic C becomesbetter signature
Sneden, Preston, & Cowan 2003, ApJ
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Note similarities of Fe-peak lines
versus disparities of the Ba and Pb lines
The “non-variable” spectrum is the mean
of three stars
CS 29497-030 = FBS (B-V)0 = 0.30
CS 29497-030 = FBS (B-V)0 = 0.30
ELABORATION
Sneden, Preston, & Cowan 2003, ApJ
Lead-rich binary CS 29497-030
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The “non-variable” spectrum is the mean of
three stars
Question:Is this a FBS?(B-V)0 = +0.30(U-B)0 = - 0.14[Fe/H] = - 2.6
CS 29497-030 = FBS (B-V)0 = 0.30
CS 29497-030 = FBS (B-V)0 = 0.30
MSTO color vs [Fe/H]
Every FBS has its own red color boundary
Lead-rich binary CS 29497-030
Answer: Yes
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One solution to the red color boundary problem for FBS:Use [Fe/H] to assign MSTO boundary star-by-star
Question:Is this a FBS?(B-V)0 = +0.40(U-B)0 = - 0.14[Fe/H] = - 2.2
Answer: No
MSTO color vs [Fe/H]
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neutron/seed ratio decreases
X = IA pop = BS pop
x
Orbit dimensions, RGB, AGB mass transferFBS binaries ( ): n-capture normal abundances (low [C/N])
mass transfer only during RGB evolution
FBS binaries ( ): n-capture over-abundances (low [C/N])mass transfer during RGB & AGB evolution
FBS single (X): n-capture normal abundances (high [C/N])
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FBS PULSATORS
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Pulsation like this would produce chaos in FBS binary RV curves,so we know that such pulsators are rare among FBS binaries.
30 km
/s
1 hour
ORBIT
PULSATION
ΔV ~ 0.1 mag.
Shift due toorbital motion
Preston & Landolt 1999 AJ
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30 km
/s
1 hour
Conclusion: Such pulsation is rare among metal-poor FBS(like 1/42 = 2 or 3 %) although most FBS lie in instability strip.
ORBIT
PULSATION
20 km/s
Preston & Landolt 1999 AJ
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HADS confined to narrow band in the instability strip.McNamara (1997), Petersen & Dalsgaard (1999)Kepler data confirm (Balona & Dziembowski 2011)Pulsator fraction: ~ 0.5 in central band < 0.5 elsewhere in instability strip
Sct instability strip
McN
amar
a’s
field
sta
rs
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Poretti et al. 2008, ApJ
RR Lyraes fill their instability strip, but SX Phe stars in Fornax II probably are confined to McNamara’s HADS strip.
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RR Lyraes fill their instability strip, but SX Phe stars in Fornax II probably are confined to McNamara’s HADS strip.
Poretti et al. 2008, ApJ
RR Lyr
SX Phe
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STARS THAT DON’T FIT
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2500 3000 3500 4000 4500 5000 5500
Julian Date
-60
-50
-40
-30
-20
-10
0
10
20
30
RV
(km
/s)
TY Gru 2003 - 2010
C & s-process rich stars that don’t fitC & s-process rich stars that don’t fit
1 km/s
20 years
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2500 3000 3500 4000 4500 5000 5500
Julian Date
-60
-50
-40
-30
-20
-10
0
10
20
30
RV
(km
/s)
TY Gru 2003 - 2010
C & s-process rich stars that don’t fitC & s-process rich stars that don’t fit
After so many years of this– NADA!
1 km/s
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2500 3000 3500 4000 4500 5000 5500
Julian Date
-60
-50
-40
-30
-20
-10
0
10
20
30
RV
(km
/s)
TY Gru 2003 - 2010
C & s-process rich stars that don’t fitC & s-process rich stars that don’t fit
After so many years of this– NADA!
1 km/s
Tengo 82 anos – no mas para mi. I quit!
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