J/MNRAS/448/3608 Titius-Bode-based exoplanet predictions (Bovaird+, 2015)
Using the inclinations of Kepler systems to prioritize new
Titius-Bode-based exoplanet predictions.
Bovaird T., Lineweaver C.H., Jacobsen S.K.
<Mon. Not. R. Astron. Soc., 448, 3608-3627 (2015)>
=2015MNRAS.448.3608B 2015MNRAS.448.3608B (SIMBAD/NED BibCode)
ADC_Keywords: Stars, double and multiple ; Planets
Keywords: planets and satellites: detection
- planets and satellites: formation -
planets and satellites: terrestrial planets - planet-disc interactions
Abstract:
We analyse a sample of multiple-exoplanet systems which contain at
least three transiting planets detected by the Kepler mission ('Kepler
multiples'). We use a generalized Titius-Bode relation to predict the
periods of 228 additional planets in 151 of these Kepler multiples.
These Titius-Bode-based predictions suggest that there are, on
average, 2±1 planets in the habitable zone of each star. We estimate
the inclination of the invariable plane for each system and prioritize
our planet predictions by their geometric probability to transit. We
highlight a short list of 77 predicted planets in 40 systems with a
high geometric probability to transit, resulting in an expected
detection rate of ∼15%, ∼3 times higher than the detection rate of our
previous Titius-Bode-based predictions.
Description:
In this paper, we perform an improved Titius-Bode analysis on a larger
sample of Kepler multiple-planet systems1 to make new exoplanet
orbital period predictions. We use the expected coplanarity of
multiple-planet systems to estimate the most likely inclination of the
invariable plane of each system.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablec1.dat 71 77 77 planet predictions with a high geometric
probability to transit (Ptrans≥0.55)
in 40 Kepler systems (subset of table C2)
tablec2.dat 71 228 All 228 planet predictions in 151 systems
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See also:
V/133 : Kepler Input Catalog (Kepler Mission Team, 2009)
Byte-by-byte Description of file: tablec1.dat tablec2.dat
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Bytes Format Units Label Explanations
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1- 8 A8 --- Name System name, KOI-NNNN
11 I1 --- Nins [0/6] Number of planet inserted in the system
13- 17 F5.1 --- Gamma ?=- Measure of the fractional amount by which
the chi22/d.o.f. improves, divided by the
number of planets inserted (1)
19- 22 F4.1 --- DGamma ?=- DGamma=(Gamma1-Gamma2)/Gamma2 (2)
24- 28 F5.2 --- chi2/dofi ?=- Chi2/d.o.f value before planets
are inserted
30- 33 F4.2 --- chi2/doff ?=- Chi2/d.o.f value after planets
are inserted
35 I1 --- Np [1/7] Inserted planet identification number
37 A1 --- n_Np [E] E: planet is extrapolated (3)
41- 46 F6.1 d Per Period
48- 52 F5.1 d e_Per rms uncertainty on Per
54- 57 F4.2 AU a Semi-major axis of the planet
59- 61 F3.1 --- Rmax Maximum radius in Earth radius (4)
63- 66 I4 K Teff Effective temperature
68- 71 F4.2 --- Ptrans probability to transit
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Note (1): Gamma=[(chi2i-chi2f)/chi2f]/nins2, where chi2i and chi2f
are the chi2 of the Titius-Bode relation fit before and after planets are
inserted, respectively, while Nins is the number of inserted planets.
Note (2): DGamma=(Gamma1-Gamma2)/Gamma2 where Gamma1 and Gamma2 are the highest
and second highest Gamma values for that system, respectively
(see Bovaird & Lineweaver, 2013MNRAS.435.1126B 2013MNRAS.435.1126B).
Note (3): A planet number followed by E indicates the planet is extrapolated
(has a larger period than the outermost detected planet in the system).
Note (4): Rmax is calculated by applying the lowest SNR of the detected planets
in the system to the period of the inserted planet. See equation (7).
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 15-Sep-2015