F. Peery,. Jr. Astronomy. Programs. Computer. Sciences. Corporation. Space. Telescope. Science. Institute. Astronomy. Department. Indiana. University. Dept.
t
/
245
N89-10729 PR_EDING
PAGE
BLANg
COMPANIONS
Thomas
B. Ake,
Astronomy Computer Space
TO
NOT
PECULIAR
Programs
Sciences
Telescope
Astronomy
Corporation
Science
Indiana
recent
peculiar
red
and HR emission
1105. lines
continuum.
observations
that
to the
indicating
companion,
other
hand,
1982,
no
C IV was
appears
to have was
strong,
II1/. 303
UV flux
may
from
temperature
a highly
discerned
increasing
be
a
AND
HR
Benjamin
Dept.
Department
F. Peery,
and
Howard
occuring
illuminated IUE data
when
by were
component
the
side
of the
but
of 3 in 1987
been
discovered
were
undertaken
Ori.
The UV,
be ruled
without
S-star
first
two
show
no
the
third
has
heterogeneous histories.
One
s-process
giants
be interacting the
Tc but
been
found
correlation
group
of objects
with
different
group
of these,
closely
related
thus may have been Under this scenario, PRG,
but
once
was
went
since the in the UV
pulsating
PRG
of the
have
white
dwarf
state,
from
Since
HR
363
Stellar
away.
(S3-1-/2-) Radial
on its
except This
latest
in deep appear
to
to K-M
giants
and
primary reflects elements
compaation
should
Little et al (Ref. Tc-deficient stars Two
surveys
been
published
A Decade
for
have
been
searched
2). ff the above scenario should be binaries with WD (refs.
companions 3-4)
of UV Astronomy
and
of the companions
wtth IUE,
in the
as being
Ake
Proc
while
Tc holds.
o I Ori
is
We report
variations,
and
is not
in
is affected
only
for
apparent.
Compared
emission
is suggestive
The
as Tc
observations corresponding
stronger
points,
S stars
to a few
Celebratory
stars
M giants
existence
is correct, the WD secondaries. MS and
the be
the
stars
Since
may
an
prominent
(Ref.
7).
red
The
obvious.
are
feature
hit
re-extraction
splitting other
is not
chromospheric
In Figure
temperature, as noted
1 we show 7 Cru
from
spectrum
363 have
has
is too
high
of a chromosphere
noisy
a composition
undergone similar
(M3
in III).
dispersion are of the
for positive
dissimilar
convective to the
at
that
by our
giants,
of
as is typical
et al (Ref. 8). While there in the HR 363 data at some the
HR
are
removed
not
lines
in general
based
or period
with a Gaussian and emission fines
by a cosmic-ray
of similar
Carpenter excursions
orbit
4) determined
Si H 1808/1817
but
emission
automatically
1815
to other
by
and
no
we have reobserved it with a the resultant spectrum after
partially
normal
an M giant
of the
Tc is by
been
since
such
be a
(Ref.
of
binary,
of a degenerate secondary based due to the importance of this
S I + Si II of M giant
that now
and
exposures
comparison
Catalogue
but
Johnson
uni'ortunately has
General
a spectroscopic
hits and reprocessing A low level continuum
technique
these
that
noted
velocity
extraneous routine.
probably 1). a
that
itself
that
1815
star.
list of PRGs
in
lines.
363
on the binary hypothesis, exposure. Figure 1 shows
confirmation. The
was
Velocities
S I + O I 1300
Tc,
a companion
the
its composition
companion,
decayed (WD)
phase.
evolutionary
of considerable than
lines
variable in the UV, HD 35155 and HR
binaries with
2. HR
removing extraction
C are a
binaries in the past (Ref. primary did not evolve into
by material
this
peculiar
S, SC and
without
to Ba II stars
polluted
a thermally should
stars but
mass-transfer the current
through
phase
the
overabundances
emission temperature
primary
the
MS,
element
be more
that
strong
no high
to be.
upper limit on the luminosity on a quick SWP survey, but
of type
in the discovery HR 1105 and o 1
on another Tc-poor S star, IIR 363, and HR 1105 is also a UV variable as HD 35155
was established.
apparent
have
Tc but
observations or
have resulted HD 35155,
mass-transfer
expected
presumably
(PRGs)
These
abundance
with
out.
increasingly red
5-6).
to Tc
1986
object longer
abundance
(refs.
regard
while
may and
has
by
serendipitously
here observations demonstrate that
1. INTRODUCTION
It is becoming
Astronomy
liD 35155 also has been noted to be higtdy both in the continuum and the lines. Thus
not,
UV companion.
system,
the companion faces the Earth, but taken over 3 orbits, a secular change
cannot
Jr.
University
prominent lines of Si IIl], C IIl], O III], Si IV and N V. Using orbital parameters, these observations are consistent with high activity
1105
of Physics
University
1105
emission
variable for this
by a factor
R. Johnson
the
that this is an interacting system recently occurred. HR 1105, on the
UV
flux
far
contribution
no high
S-type
binaries,
the
a possible
IIR 363
indications of binary nature, but of three stars with hot secondaries:
of IIR 363 shows and a trace of
M giants,
but
lines are seen to indicate where mass-transfer has
In
Tc-deficient
spectroscopic
A 675 min SWP exposure of O I 1304 and Si II 1812
larger,
dwarf
of two
are also
Compared
relatively white
IUE
giants
GIANTS:
Institute
ABSTRACT
We report
F1-LMFA)
RED
Hollis
IIl
,
from
mixing,
M giants
the
should
not
assumed.
have have
Symposium,
Since
GSFC,
we are looking
Greenbelt,
USA,
for a hot
12-15
April
companion
to HR
1988, ESA SP-281,
363,
we are
Vol. 1 (June
1988)
246
_
- IIIII
T B AKE,
H R JOHNSON
1
r
& B F PEERY
1
T
i"
1
r
1
E
_
2
_
0
-
3
0 i _"
Cru
E
cl
X
2
S
co?
._x
I
C
17
I
0
I
Figure
1. SWP
interested
in whether
compared
to other
on
the
1200
1300
argue to
that
the
these
1400
the
light
Basri
(Ref.
10)
25%
of the
flux
UV
and
1500
model
for
find
1600
in single in interpreting
the
SWP.
M giants the
is below
is real data
is not
due
observations
in
HR 363
derived
is about
and
one
revision than
Thus
the
must
as evidence
added by
exercise
for
flatness
of the-spectrum
by measuring
A, converting
rex600
= -2.5
for
is not present. the upper limit the
it to
average
- 21.1,
1. Average
Fluxes
363,
a WD
HR Type
V E(B SWP F,xp
- V) Number Time
(rain)
Observer (m16oo-
V)o
363
$3+/2
flux in the scale
and
using
at
1600
the
1250
the
by colors
(Ref.
bluer
than
SWP
the
7 Cru M3 III
p Per M4
II-III
the
If the should
(see Ref. spectrum
added then
flux have
we UBVRI
color
curve
and
for
indicating
for
HR
there
continuum
Mv=ll.2,
for
is
type,
the
entire
we derive
magnitude
V colors
data
which
spectral
that
M stars
region.
-
The published
their
white
to compute
mlB00
values,
Note
363 is
in HR
but
the flux
upwards
at the
4). If we assume that HI{ 363 comparable to the M giants, we
yields
Mv=ll.7
a flatter
for
energy
3. HR
the
companion,
distribution.
Giants
g Her M6 III
1.62
3.2
5.05
0.05 32472
0.00 5891
0.03 32553
0.0O 1387
90
249
154
Ake
Sarmer
Ake
Wing
9.63
10.24
10.05
10.00
1105
to 11o5
whose
resultant
Red
for
11).
to a companion,
would
the
comparing
field
primary
M giants.
reddening
mean
of this
identified.
for
of the
1 we present
with
in the
are
determinations
tabulated
Eggen
in 7 Cru
3 late-type
M giants
0.5 mag
that
HR
computing
A for
2000
with
region
by
1900
magnitude
In Table
shortest wavelengths has a chromospheric find
6.43
675
similar
the
from flux
($3.5/2)
is a 596
secondary
was
obtained
2 SWP
the
day,
same
day
first
exposures
the
longer
spectroscopic
reported
of 20 min. one
binary
by Peery
taken
and
after
(ReL
(Ref.
6).
87 rain.
12)
He had
duration
C IV emission
We
have
variability
spectra
with
2 we present centered phases The
obtained
2 other
of this
object.
the stronger the
from recent
state than December
emission
integrated
in the relatively
observations
In Figure line
line
lines fluxes
determination
observations
have
caught
are the
was was
can confirm
2 we show
plots
of the
identified,
and
in Table
and
free region
Griffm's
and
on
was
fotmd in the first image. Interestingly a 20 rain. exposure obtained by O'Brien and Johnson in 1982 and no emission seen.
Star
absolute
for
363 is due
the Spectral
-
is unclear.
In Ref. 4 we describe a method to the luminosity of a hot
a magnitude
log(f18oo)
Table
HR
with
the
well as for
for a WD far
color
for
obtained
lines
lines
limit.
363 as
corrected
more
5%.
the upper
7)
calculated
in the
weaker
and
which
Tell > 15000K for determining
1950
s,
1800
Chromospheric
of the
(Ref.
companions.
secondary
J_
1700
7 Cru.
HR
rough
9) have
contribute
likely
been
because
We have
star
the reality
dwarfs
chromospheres
et al (Ref.
it cannot
A, and
caution
By the
II
(A)
m16o0 -- V
has
Sanner
as prescribed
that
little Prom
lower
M3 III
work
perhaps and
the where
flux
for M giants
the
Basri
and 363,
much
SWP.
region
paper,
continuum
some
in the
from
363
giants,
Stickland
contribution
at 1900
been
continuum,
light
arises
their
has
of cool
in this
but
scattering
scattered
spectra
HR
for HR
continuum
there
underlying
continuum
Since
an improved
line
PRG showr,
is additional While
contamination,
scatter,
stars.
are
scattered
of the
grating
of the
there
general
about
estimates
spectra positions
stars.
emission the
of concerns
i +
Si
_
Corresponding
about
s
II
II
Wovelength
said
+
Fe
0
1 100
done
I
a continuum at
also
1460/_.
flux Orbital
indicated.
system
in a higher
previously seen, with a subsequent decline 1987 to March 1988 in both the continuum
from and
COMPANIONS TOPECULIAR RED GIANTS HR363& HR1105 2O
247
I
N
V O
I Sl
15
IV
C
SWP
IV
32552
Sl
m O
III]
III 1 Si
II
oD
E ยข9
10 h,t ? SWP
33059
SWP
27678
x X Z3
5
_
[
f
o
I
11Q0
1200
1 300
1400
1 :500
1 600
Wavelength Figure
2. Temporal
5 x 10 -14
emission
lines.
together,
with
the
In general, little
continuum
1987.
essentially
These
associated rather apparent
was
the
continuum
that
the
same
analysis
of the
ratio
of tiffs
system
was
not but
(miss0
in the
redder,
system,
The
1986
are
continuum
and
-
V)
Finally
lines
such
the
4. DISCUSSION
1105,
and
brightness
spectroscopic are
quite
and
binary different
HR
PRGs, and
the
1105 their
evidence
are
Tc-deficient
characteristics for
the
in the
far
by the should
UV
mass-transfer
Table
the
2. IUE
Observations Flux
or a hot
companion. be correlated
points
at which
of HR
(x 10 -13
is not
and
HR
the
outer
In the with the
flux
currently
is not
but indicate
of the
have
SWP
No.
been
1105
ergs/cm2/s)
1982 1986
Aug 31 Feb 7
17816 27678
1987
Dec
17
32552
6
33059
1988Mar
Overexposed
Phase 4.057
NV
OI
SiIV
CIV
SilII]
CIIII
6.163
1.38
1.71
2.34
9.27
0.18
0.49
7.302 7.436
7.60 3.80
3.02 2.69
6.17 1.75
> 27 a 11.7
2.03 1.12
1.78 0.92
as these between
primary
are the
heated
the observed changes In Figure 3 we show
f1460
Date
that
observed.
such
a stream
atmosphere
as with clear.
directly
systems
last two cases, orbital phase.
an
is not
continuum
for
a
1105.
is present,
secondary,
is from emission
UV radiation
of the
observations
is even
for a brighter UV
tiffs
to
chosen. the
temperature
companion
around
is required
M giants
if excess
M giants,
Further
giants
opt
that
of the radiation
disk
type
35155
of the
of a WD
locations
red
companion
variability
components, 363
a hot
the
objects were we find that
of high
HD
with
be inferred.
would
that
source
photosphere
only
earlier
standards
the
accretion
can
of other
absence
clearly
abundance
comparison
comparison Sanner data,
symbiotics,
Possible an
HR
363
K and
like
by are indicated.
current
on
we note
the
system
For Hit
the
to be variable.
The
both
of their
as C IV indicates
interacting
March
for other
offset
slopes
chromospheres
color
companion,
are
Based
to HR
so using
WD
the
While
origin
is mixed.
companion.
lines
plots
confirm that appropriate From the Stickland and
to the
weak.
appear
is
20Q0
1900
continuum
the
companion
in the
Feb
for
a WD
but in 1986 N V is weaker and the is < 1. Thus on a longer time scale,
conditions
hypothesis
and
bluer
III]
1800
Successive
is slightly
by a decrease
in the
region.
are labelled
peculiarities
decline
variations
SWP
features
scale
of the
is somewhat
the
in the
and
Compared
some
1105
emission
of different
energetics reduced
HR
strengths
Si III]/C
of lines
region.
however, exposure
1988 observations, Si III]/C III] ratio physical
emitting
A is nearly
line
argue
luminosity
1460
continuum
sensitive
total
in 1986,
and
ratios
observations
size of the
at
density as are
in the
although
flux
The
PRG
Prominent
relative
the
a change
observation seen,
lines
with the
of the each.
in the
although
unchanged,
excitation.
the
change
slope,
in December
variation
ergs/cm2/sec/A
1 700 (A)
(ergs/cm2/s/_) 8.6a(-15) 1.60(-14) 3.01(-14) 1.63(-14)
made.
There
is
T B AKE,
248
H R JOHNSON
& B F PEERY
5. REFERENCES
1.
Smith
V E & Lambert
2.
Little
S J, Little-Marenin
Astron
17816
=0 27678
__
Figure 3. Motion of the HR 1105 system center of mass. Phases at been taken are marked.
S-type which
J, 94,
3.
Smith
4.
Ake
5.
Johnson
6.
T B & Johnson
a general the
relationship
hemisphere
was nearly seen
in
plane past
1982)
of the
on,
while
occurred sky.
the
But
data
the correspondences variations cannot required
the
of the primary
face
year,
in that
except
state
illuminated
the
when
highest
lowest
for
the
was collected
by the
phase
the primary
occurred
and
(i.e.,
observations
7.
emission
York:
Peery
B F Jr 1986,
if the
changes
are
made orbital
actually
obtaining specialized supported
acknowledge
the
assistance
of the
so
8.
9.
periodic.
IUE
staff
these observations and the GSFC RDAF in the extraction routines. The work by T. B. A. is by
NASA
grant
NAS
5-28749.
Astrophys
T B 1983,
in
eds.
in
977.
J, _27,
Cool
Stars,
S L Ballunas
214.
Stellar
& L Hartmann,
p. 362.
New
Insights
Observations p.
J, 94,
with
in Astrophysics: IUE,
ed.
E l%olfe,
117.
D J & Sanner
F 1981,
Mon
Carpenter
K G, Pease
J E, Stencel
Johansson
S & Wing
Not
Roy
Astr
R E, Brown
A,
Soc,
791.
in the
cycles:
6. ACKNOWLEDGEMENTS
We gratefully
SP-263,
Astron
H R 1988,
Springer-Verlag),
of UV
Stickland 197,
of the
are somewhat suspect since secular be ruled out. Further observations are
to confirm
W H 1987,
companion
no
was in front
at different
D L 1987,
the Sun,
(New
ESA
when
I R & Bauer
H R & Ake
8 Years
preprint.
981.
V E & Lambert
Systems,
primary about the SWP spectra have
D L 1988,
Basri
G,
144,
161.
Clarke
G 1985,
R F 1988,
J T & Haisch
10.
Basri
NASA
11.
Eggen
O J 1972,
12.
Griffin
R F 1984,
IUE
Astrophys B M 1985,
Newsletter,
Astrophys
J, 177,
No.
479.
in Observatory,
104,
224.
J, submitted. Astron
Astrophys,
28, p. 58.
