SLIDE 1
1
2
Rossiter-McLaughlin (RM) effect
All lines undergo the same kind of the distortion (up to the variations
- f the limb darkening
law in different lines)
UX Ori: V. Grinin, I. Potravnov, 2013 for RZ Psc
- J. Winn, 2011
Inhomogeneous eclipses in the UX Ori type stars Suslina E., Dodin - - PowerPoint PPT Presentation
Inhomogeneous eclipses in the UX Ori type stars Suslina E., Dodin - - PowerPoint PPT Presentation
1 Inhomogeneous eclipses in the UX Ori type stars Suslina E., Dodin A. Sternberg Astronomical Institute 2 Rossiter-McLaughlin (RM) effect All lines undergo the same kind of the distortion (up to the variations of the limb darkening law
SLIDE 2
SLIDE 3
3
Variability of LSD profiles
CQ Tau
RY Ori
PAR 1414
- F. Villebrun et al., 2019
SLIDE 4
4
CQ Tau
SME (Piskunov, Valenti, 2016)
SLIDE 5
5
22.12.2012 25.12.2012 22.12.2012 28.12.2012 22.12.2012 29.12.2012
All lines show the same kind of distortion, as expected for RM effect:
ESPaDOnS
SLIDE 6
6
Modelling
– SME – rigid rotation of spherical star – standard extinction law
SLIDE 7
7
EW
EW
EW EW
SLIDE 8
8
SLIDE 9
9
SLIDE 10
10
SLIDE 11
11
SLIDE 12
12
The differences in lines give the information about cloud’s shape The pattern of variability gives information about the direction
- f movement
SLIDE 13
13
Modelling
Due to the inhomogeneous eclipses the line profiles show complex shape with narrow features – as was observed
CQ Tau:
22.12.2012 25.12.2012
CaI 6122
SLIDE 14
14
Consequences of inhomogeneity
Radial velocity and v sin i distortion Parameters of the star ( ) are
slightly distorted due to differences in limb darkening in weak and strong lines:
Star’s properties are affected:
(
EW weak EW strong)0 ≠( EW weak EW strong)eclipse
mic eff
V g, , T log
SLIDE 15
15
Dust properties:
Inhomogeneous eclipses are tend to be more
grey, leading to incorrect conclusion about the mean size of dust grains:
(Natta, Panagia, 1984)
λ A
f + f
2.512 1 2.5log
Consequences of inhomogeneity
0.9 = f 3 = A
V
Cardelli, Clayton & Mathis, 1989 , for standard extinction
SLIDE 16
16
Consequences
Distortions observed in absorption lines
should be present in the emission lines:
A simulated Ha image of accreting CTTS with an outflow (Kurosawa et al., 2006):
The same, but with clouds:
SLIDE 17
17
Conclusions
- 2. Differences in line profiles give an
- pportunity to map the clouds
- 1. Obscuring clouds are structured on the
scales of stellar radii
- 3. Series of observations within one night
will make the study of clouds movements possible
SLIDE 18
18
Thank you for your attention!
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