SLIDE 1 RW Aur binary: asymmetrical effect of the fly-by
- n the inner regions of circumstellar discs of the
components
Lamzin S.,1 Dodin A.,1 Petrov P., 2 Safonov B., 1, Takami M.3, Tatarnikov A.,1 Vozyakova O. 1
1 – SAI MSU, Russia, 2 – CrAO RAS, 3 – Institute of Astronomy and Astrophysics, Academia Sinica
SLIDE 2 Young binary system RW Aur
D = 163 pc, d ≈ 1.5 arcsec ≈ 240 au RW Aur A RW Aur B L* ≈ Lac ≈ 1.5 Lʘ L*=0.6 Lʘ , Lac << L T
eff ≈ 5000 K
(K2) 4100 (K7) R ≈ 1.9 Rʘ 1.2 Rʘ M ≈ 1.4 Mʘ 0.8 Mʘ
SLIDE 3
AAVSO V-band light curve of RW Aur A+B from September, 2009 to September, 2019
SLIDE 4
Polarization-magnitude dependence For RW Aur A Eclipses are produced by dusty disk wind !!!
Dodin et al., 2019
SLIDE 5
Dai . et al. (2015) Fly-by model
SLIDE 6
Jet of RW Aur A (Berdnikov et al., 2017)
A B
Interactions of components in double systems trigger accretion events that produce powerful outflows (Reipurth , 2000) .
SLIDE 7
But RW Aur B also has disk, so what occurs with it ? Rodriguez et al., 2018
SLIDE 8
SLIDE 9
Fast dimmings: up to V ≈ 1m during one day
SLIDE 10
U,…, J and H,K histograms are different
SLIDE 11
Optical and NIR colour-magnitude diagramms are also different Blueing effect ?
SLIDE 12
fades polarization increases (up to 3 % in V )
disc scattering ? V R I
SLIDE 13
Conclusion 1 RW Aur B is UX Ori type star, i.e. its photometric variability occures due to eclipses by (gas-)dust clouds Dusty wind as in the case of RW Aur A ? Probably not…
SLIDE 14 T
eff ≈ 4100 +/- 50 K
SLIDE 15
SED of RW Aur B disk
SLIDE 16
1) Accretion signatures in H Balmer lines. EWHa ≈ 4 A in our spectra, but Duchene et al. (1999) observed EWHa ≈ 43 A . 2) Powerful chromosphere in He I and Ca II lines; 3) No wind signatures -- e.g. [O I].
SLIDE 17
RW Aur B has no jet !
A B
But why ???
SLIDE 18
RW Aur B: LX ~ 10-3 Lbol , powerful corona The star has magnetic field !?
Gunter et al., 2018
SLIDE 19
3D MHD simulations of jet launching from disks in binary systems (Sheikhnezami & Fendt 2018) suggest a critical angle between disk plane and orbital plane of somewhat above 10 degrees beyond which a jet cannot persistently be formed out of a disk wind. Wurster & Bate (2019) also found that bipolar outflows are launched in only 17 models out of 105, and these models have strong magnetic fields that are initially parallel to the rotation axis. It supports the idea of Fendt & Zinnecker (1998) who consider a certain degree of axisymmetry as essential ingredient for jet launching.
SLIDE 20
Rodriguez et al. (2018) found that i ≈ 56 o in the case of RW Aur A i ≈ 68 o in the case of RW Aur B i.e. the disks of A and B components misaligned by 12o
SLIDE 21 Conclusion 2: Possibly RW Aur B has no jet due to relatively large inclination
- f inner regions of its disk
to the orbital plane
SLIDE 22 Thank you for attention !
The study of SL, AD and BS was conducted under the financial support
- f the Russian Science Foundation Public Monitoring Committee
17-12-01241.
