2011A&A...528A..53B


Query : 2011A&A...528A..53B

2011A&A...528A..53B - Astronomy and Astrophysics, volume 528A, 53-53 (2011/4-1)

Transit timing variations in eccentric hierarchical triple exoplanetary systems. I. Perturbations on the time scale of the orbital period of the perturber.

BORKOVITS T., CSIZMADIA Sz., FORGACS-DAJKA E. and HEGEDUES T.

Abstract (from CDS):

We study the long-term time scale (i.e. period comparable to the orbital period of the outer perturber object) transit timing variations (TTVs) in transiting exoplanetary systems that contain another more distant (a2≫a1) planetary or stellar companion. We give an analytical form of the O-C diagram (which describes such TTVs) in a trigonometric series, which is valid for arbitrary mutual inclinations, up to the sixth order in the inner eccentricity. We show that the dependence of the O-C on the orbital and physical parameters can be separated into three parts. Two of these are independent of the real physical parameters (i.e. masses, separations, periods) of a concrete system and only depend on dimensionless orbital elements, so can be analysed in general. We find that, for a specific transiting system, where eccentricity (e1) and the observable argument of periastron (ω1) are known, say, from spectroscopy, the main characteristics of that TTV, which is caused by a possible third-body can be mapped simply. Moreover, as the physical attributes of a given system only occur as scaling parameters, the real amplitude of the O-C can also be estimated for a given system, simply as a function of the m3/P2 ratio. We analyse the above-mentioned dimensionless amplitudes for different arbitrary initial parameters, as well as for two particular systems, CoRoT-9b and HD 80606b. We find in general that, while the shape of the O-C strongly varies with the angular orbital elements, the net amplitude (departing from some specific configurations) depends only weakly on these elements, but strongly on the eccentricities. As an application, we illustrate how the formulae work for the weakly eccentric CoRoT-9b and the highly eccentric HD 80606b. We also consider the question of detection, as well as the correct identification of such perturbations. Finally, we illustrate the operation and effectiveness of Kozai cycles with tidal friction (KCTF) in the case of HD 80606b.

Abstract Copyright:

Journal keyword(s): methods: analytical - planets and satellites: individual: CoRoT-9b - planets and satellites: individual: HD 80606b - methods: numerical - planetary systems - binaries: close

Simbad objects: 11

goto Full paper

goto View the references in ADS

Number of rows : 11
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 * bet Per EB* 03 08 10.1324535 +40 57 20.328013 1.70 2.07 2.12 2.08 2.11 B8V 1163 2
2 * lam Tau EB* 04 00 40.8157175 +12 29 25.225937 2.66 3.29 3.41 3.44 3.53 B4IV 335 0
3 WASP-12b Pl 06 30 32.7966788910 +29 40 20.266334158           G0 598 1
4 HD 80606b Pl 09 22 37.5769478105 +50 36 13.434928660           ~ 284 1
5 HD 80606 PM* 09 22 37.5769478105 +50 36 13.434928660   9.78 9.00     G8V 292 2
6 HD 80607 PM* 09 22 39.7367015092 +50 36 13.952617706   9.937 9.070     G5 85 2
7 BD-07 3477 HS* 12 44 20.2386520980 -08 40 16.848587212   10.46 10.594 10.895   sdB2VIIHe3 260 1
8 V* QS Vir EB* 13 49 52.0031855330 -13 13 37.001934702 14.27 14.98 14.40 14.37   DA3+dM 126 1
9 V* CM Dra BY* 16 34 20.3299130309 +57 09 44.365524588   14.50 12.87 10.85 9.26 M4.5V 412 0
10 CoRoT-9b Pl 18 43 08.8101080314 +06 12 14.912939950           ~ 61 1
11 V* V391 Peg HS* 22 04 12.1044101613 +26 25 07.820507559   14.41 14.61 15.00   sdB 101 2

To bookmark this query, right click on this link: simbad:objects in 2011A&A...528A..53B and select 'bookmark this link' or equivalent in the popup menu


2021.07.31-09:01:09

© Université de Strasbourg/CNRS

    • Contact