Download Semin2007a3

Rotational Velocities of the Red
Giants in Symbiotic Binary Stars
Радослав К. Заманов
(Институт по Астрономия, Българска Академия на Науките)
в сътрудничество с:
M.F. Bode (Liverpool, UK),
C.H.F. Melo (ESO, Chile)
A. Gomboc (Ljubliana, Slovenia),
R. Bachev, I. K. Stateva, R.Konstantinova-Antova (Sofia, Bulgaria)
October 2007
Symbiotic binary star = Red Giant + White Dwarf
Symbiotic stars are interacting binaries consisting of red giant
transferring mass onto a white dwarf.
We are investigating the projected rotational velocities of the
mass donors. Our aims are:
•
•
•
To check theoretical prediction that the red giants in these
binaries are co-rotating (for objects with known periods).
To perform comparative analysis and to check if they are
faster rotators (comparing with isolated giants and those in
wide binary systems).
To give clues for binary periods, individual mass loss rates,
select candidates for X-ray observations.
Observations:
40 symbiotic stars have been observed with the 2.2m telescope
(ESO, La Silla) + FEROS spectrograph at resolution 50000.
Our sample:
 All objects from the Symbiotic star catalogue with
0h<R.A.<24h, Declination < 00, and brighter than V< 12.5
mag.
 From literature -12 northern symbiotics.
 Our sample is flux limited, there should be no biases in
rotation.
ESO – La Silla
ESO La Silla - 2.2 m telescope
Observations:
the 2.2m telescope + FEROS spectrograph
-
resolution 48000;
-
dispersion=0.03 A/pixel
wavelength coverage:
3600 – 8900 AA in a single exposure
- signal-to-noise ratio = 50; V=12 mag; exposure=30 min
Fig. Theoretical spectrum
and spectra of a few
symbiotic in the near IR:
wavelength 8760-8850 AA
Fig. Numerical mask and
spectra of a few symbiotic in
Wavelength interval 87608850 AA.
To measure the projected rotational velocity (v sin i)
we used the CCF method and numerical template.
The width of the CCF is connected (calibrated for
FEROS) with the v sin i.
Two examples of the Cross-Correlation Function and the fitting gaussian.
Left – AS 316 – v sin i = 9.8 ± 1.5 km/s
Right – rapid rotator V417 Cen – v sin i = 75 ± 7.5 km/s
Fig. Check of our methods.
The measurements of v-sin-i
with FWHM and CCF
methods are in good
agreement.
The rotational period of the
red giant versus the orbit
period for 16 symbiotic stars
in our sample with known
orbital periods (all they are
S-type).
The solid line represents
synchronization (Porb=Prot).
Among these 16 objects there
are two, which deviate
considerably from corotation: CD-43 14304 and
RS Oph. There are doubts
that v sin i of CD-43 14304
could be wrong. RS Oph
seems to be the only
symbiotic system which is
not synchronized.
D’-type symbiotics are characterized by an earlier spectral type
giant (F-K) and lower dust temperatures. Rotational velocities
have been measured for five such stars (Zamanov et al. 2006).
Four of these five objects appeared to be very fast rotators,
compared with the catalogues of v sini for the corresponding
spectral types. At least three of them rotate at a substantial
fraction (≥ 0.5) of the critical velocity. Hence, in D’-type
symbiotics, the cool components rotate faster than the isolated
giants of the same spectral class (as predicted by Soker 2002).
As a result of rapid rotation, they must have larger mass loss
rate, probable enhanced in the equatorial regions. In addition, as
a result of the fast rotation, magnetic activity is expected to exist
in these giants.
Fig. v sin i versus the spectral type.
Symbiotic stars – red crosses, black –
single giants.
Isolated giants spectral classes K2-K5 III
(238 objects from catalogues of v sin i)
K2-K5 III giants in symbiotic stars
(7 objects, our measurements)
Results:
238 K2III-K5III stars:
The K giants in symbiotic stars:
v sin i = 1.0 - 6.7 km/s
v sin i = 4.5 - 8.9 km/s
mean v sin i =1.70 km/s)
mean v sin i =7.42 km/s)
The Koslmogorov-Smirnov test gives a probability of 10-4 (K-S statistics =0.60)
K-giant mass donors of symbiotic stars rotate faster than isolated K-giants !!!
Isolated giants spectral classes M0-M7 III
(12 objects from catalogues of v sin i)
M0-M7 III giants in symbiotic stars
(28 objects, our measurements mostly)
isolated M giants: 1.8 < v sin i < 18 km/s
M-giants in symbio 3.0 < v sin i < 52 km/s
(mean vsini=5.54 km/s)
(mean vsini=9.07 km/s)
The tests gives a probability of 0.09-0.01 that both distributions are coming from the same
parent population.
Discussion:
The reasons for faster rotation in giants in symbiotic systems could be:
- synchronization, if the time spent by the mass-losing star on the giant branch
is longer than the synchronization time. In all symbiotic systems with orbital
period Porb ≤ 100 years tidal interaction overcomes the angular momentum
loss by the wind (Soker 2002).
- accretion during the MS phase of the present red giant: the more massive star
in the system, the present WD, had transferred material at the stage when it
had been red giant.
- backflowing material: hot component prevents part of the mass blown by the
giant from acquiring the escape velocity for the binary system. This fraction of
mass may acquire angular momentum, and if it is accreted back by the giant, it
spins-up its envelope.
- angular momentum dredge-up when convective envelope approaches the core
region of the giant.
- planet engulfment during the giant phase.
CONCLUSIONS:
•
We have measured the projected rotational velocities of 40 symbiotic stars
(v sin i) by the means of CCF.
•
Among 16 symbiotics with known orbit and rotation, there is only one (RS
Oph) which is probably not synchronized.
•
Our results show that the mass donors in the symbiotic stars rotate faster
than isolated giants. The faster rotation is undoubtfull for D’-type (yellow)
symbiotics and for those harbouring K-giant as mass donor. For those with
M giant it is not so obvious.
FUTURE WORK:
To strengthen our results, more data on M-type isolated giants and more
v sin i measurements of K-type mass donors in symbiotics are desirable. We
intend to expand our sample with northern and fainter symbiotic stars.
Open questions:
1. Is there a bimodal distribution of v sin i of the isolated giants?
2. Hen 3-1674 rotates very fast v sin i = 52 km/s
M5III - R=139 Rsun, and mass 1-3 Msun, Vcrit=40-60 km/s.
What is this object? a monster? or just an error somewhere?
3. Is there a connection between the rotation of the red giant and the density of the circum
binary nebula and mass accretion rate?
THE END
Isolated giants spectral classes K2-K5 III
(238 objects from catalogues of v sin i)
K2-K5 III giants in symbiotic stars
(7 objects, our measurements)
Results:
238 K2III-K5III stars have vsini in the interval from less than 1.0 km/s up to 6.7 km/s
with mean vsini =1.70 km/s (median= 1.50 km/s) and standartd deviation of the sample = 0.90 km/s.
The K giants of 8 S-type symbiotic stars with mass donors K2III-K5III have vsini in the interval from 4.5 up
to 8.9 km/s
with mean vsini=7.42 km/s (median=7.15 km/s) and stddev= 1.54 km/s.
The Koslmogorov-Smirnov test gives a probability of 10-6 (K-S statistics =0.60) that both distributions are
coming from the same parent population. This means that the K-giant mass donors of symbiotic stars
rotate faster than isolated K-giants.
Isolated giants spectral classes M0-M7 III
(12 objects from catalogues of v sin i)
M0-M7 III giants in symbiotic stars
(28 objects, our measurements mostly)
The isolated M giants: 1.8 km/s < v sin i < 18.1 km/s,
mean vsini=5.54 km/s (median=3.10 km/s), stddev=5.22 km/s.
The M-type mass donors of symbiotics 3.0 < v sin i < 52 km/s,
mean vsini=9.07 km/s (median=7.72 km/s), stddev=8.81 km/s.
The Kolmogorov-Smirnov test gives a probability of 0.0074 (K-S statistic =0.54) that both
distributions are coming from the same parent population. This means that from
statistical point of view the M giants mass donors of symbiotic stars rotate faster than
isolated M-giants (at confidence level 99%).
Observations:
40 symbiotic stars have been observed with the 2.2m telescope
(ESO, La Silla) + FEROS spectrograph at resolution 50000.
Our sample:
 All objects from the Symbiotic star catalogue with
0h<R.A.<24h, Declination < 00, and brighter than V< 12.5
mag.
 From literature -12 northern symbiotics.
 Our sample is flux limited, there should be no biases in
rotation.