2014AJ....147...32G

Query : 2014AJ....147...32G

2014AJ....147...32G - Astron. J., 147, 32 (2014/February-0)

Overstable librations can account for the paucity of mean motion resonances among exoplanet pairs.

GOLDREICH P. and SCHLICHTING H.E.

Abstract (from CDS):

We assess the multi-planet systems discovered by the Kepler satellite in terms of current ideas about orbital migration and eccentricity damping due to planet-disk interactions. Our primary focus is on first order mean motion resonances, which we investigate analytically to lowest order in eccentricity. Only a few percent of planet pairs are in close proximity to a resonance. However, predicted migration rates (parameterized by τn = n/|{dot}n|) imply that during convergent migration most planets would have been captured into first order resonances. Eccentricity damping (parameterized by τe = e/|{dot}e|) offers a plausible resolution. Estimates suggest τe/τn∼ (h/a)2 ∼ 10–2, where h/a is the ratio of disk thickness to radius. Together, eccentricity damping and orbital migration give rise to an equilibrium eccentricity, eeq∼ (τe/τn)1/2. Capture is permanent provided eeq ≲ µ1/3, where µ denotes the planet to star mass ratio. But for eeq ≳ µ1/3, capture is only temporary because librations around equilibrium are overstable and lead to passage through resonance on timescale τe. Most Kepler planet pairs have eeq> µ1/3. Since τn{Gt} τe is the timescale for migration between neighboring resonances, only a modest percentage of pairs end up trapped in resonances after the disk disappears. Thus the paucity of resonances among Kepler pairs should not be taken as evidence for in situ planet formation or the disruptive effects of disk turbulence. Planet pairs close to a mean motion resonance typically exhibit period ratios 1%-2% larger than those for exact resonance. The direction of this shift undoubtedly reflects the same asymmetry that requires convergent migration for resonance capture. Permanent resonance capture at these separations from exact resonance would demand µ(τn/τe)1/2 ≳ 0.01, a value that estimates of µ from transit data and (τe/τn)1/2 from theory are insufficient to match. Plausible alternatives involve eccentricity damping during or after disk dispersal. The overstability referred to above has applications beyond those considered in this investigation. It was discovered numerically by Meyer & Wisdom in their study of the tidal evolution of Saturn's satellites.

Abstract Copyright: ∼

Journal keyword(s): celestial mechanics - methods: analytical - methods: numerical - planet-disk interactions - planets and satellites: dynamical evolution and stability - planets and satellites: formation

Simbad objects: 1

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Number of rows : 1
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2024 		#notes
1 BD-15 6290 BY* 22 53 16.7325836486 -14 15 49.304052185 12.928 11.749 10.192 9.013 7.462 M3.5V 1016 1

Query : 2014AJ....147...32G

Basic data :
BD-15 6290 -- BY Dra Variable
Origin of the objects types :

(Ref) Object type as listed in the reference "Ref"
(acronym) Object type linked to the acronym according to the original reference
() Anterior to 2007, before we can link the objet type to a reference, or given by the CDS team in some particular cases

Other object types: 		* (2015ApJS,BD,...), PM* (2013MNRAS,Ci,...), BY* (2017ARep), Ro* (2012A&A), V* (V*), NIR (2MASS), MIR (WISEA)
Syntax of coordinates is : "ra dec (wtype) [error ellipse] quality bibcode" :
  • ra dec : right ascension and declination (unit and frame defined according to your Output Options)
    Grey values are increasing the original precision due to the computation of frame transformations
  • (wtype) : wavelength class for the origin of the coordinates (Rad, mm, IR, Optical, UV, Xray, Gam)
  • [error ellipse] : measurement uncertainty, on (ra,dec) if the positional angle is 90 degrees, on (majaxis,minaxis) otherwise (in mas at defined epoch in the original catalogue),
    position angle (in degrees North celestial pole to East)
  • quality : flag of quality
    • E ≥ 10"
    • D : 1-10" (and some old data)
    • C : 0.1-1"
    • B : 0.01-0.1" + 2MASS, Tyc
    • A : VLBI, Hipparcos
  • bibcode : bibcode of the coordinates reference
ICRS coord. (ep=J2000) : 		22 53 16.7325836486 -14 15 49.304052185 (Optical) [ 0.0338 0.0258 90 ] A 2020yCat.1350....0G
Syntax of coordinates is : "ra dec (wtype) [error ellipse] quality bibcode" :
  • ra dec : right ascension and declination (unit and frame defined according to your Output Options)
    Grey values are increasing the original precision due to the computation of frame transformations
  • (wtype) : wavelength class for the origin of the coordinates (Rad, mm, IR, Optical, UV, Xray, Gam)
  • [error ellipse] : measurement uncertainty, on (ra,dec) if the positional angle is 90 degrees, on (majaxis,minaxis) otherwise (in mas at defined epoch in the original catalogue),
    position angle (in degrees North celestial pole to East)
  • quality : flag of quality
    • E ≥ 10"
    • D : 1-10" (and some old data)
    • C : 0.1-1"
    • B : 0.01-0.1" + 2MASS, Tyc
    • A : VLBI, Hipparcos
  • bibcode : bibcode of the coordinates reference
FK4 coord. (ep=B1950 eq=1950) : 		22 50 34.6499284991 -14 31 14.052098435 [ 0.0338 0.0258 90 ]
Syntax of coordinates is : "ra dec (wtype) [error ellipse] quality bibcode" :
  • ra dec : right ascension and declination (unit and frame defined according to your Output Options)
    Grey values are increasing the original precision due to the computation of frame transformations
  • (wtype) : wavelength class for the origin of the coordinates (Rad, mm, IR, Optical, UV, Xray, Gam)
  • [error ellipse] : measurement uncertainty, on (ra,dec) if the positional angle is 90 degrees, on (majaxis,minaxis) otherwise (in mas at defined epoch in the original catalogue),
    position angle (in degrees North celestial pole to East)
  • quality : flag of quality
    • E ≥ 10"
    • D : 1-10" (and some old data)
    • C : 0.1-1"
    • B : 0.01-0.1" + 2MASS, Tyc
    • A : VLBI, Hipparcos
  • bibcode : bibcode of the coordinates reference
Gal coord. (ep=J2000) : 		052.0040597500243 -59.6300891766021 [ 0.0338 0.0258 90 ]
Syntax of proper motions is : "pm-ra pm-dec [error ellipse] quality bibcode"
  • pm-ra : mu-ra*cos(dec) (expressed in the ICRS system in mas/yr)
  • pm-dec : mu-dec (expressed in the ICRS system in mas/yr)
  • [error ellipse] : error major axis and minor axis (in mas), orientation angle (in deg)
  • quality : flag of quality (A=best quality -> E=worst quality, {� } =unknown quality)
  • bibcode : bibcode of the proper motion reference
Proper motions mas/yr : 		957.715 -673.601 [0.041 0.031 90] A 2020yCat.1350....0G
Syntax of radial velocity (or/and redshift) is : "value [error] (wavelength) quality bibcode"
  • value : radial velocity or/and redshift (Heliocentric frame) according to your Output Options
    (redshift may be not displayed if the data value is <0 and the database inside value is a radial velocity)
  • [error] : error of the corresponding value displayed before
  • (wavelength) : wavelength range of the measurement : Rad, mm, IR, Opt, UV, Xray, Gam or  '∼'(unknown)
  • quality : flag of quality ( A=best quality -> E=worst quality, ∼=unknown quality)
  • bibcode : bibcode of the value's origin
Radial velocity / Redshift / cz : 		V(km/s) -1.47 [0.0003] / z(spectroscopic) -0.000005 [0.000000] / cz -1.47 [0.00]
   (Opt) A 2018MNRAS.475.1960F
Syntax of parallax is : 'value quality [error] bibcode'
  • value : parallax value
  • quality : flag of quality (A=best quality -> E=worst quality, {� } =unknown quality)
  • [error] : mean error
  • bibcode : bibcode of the parallax reference
Parallaxes (mas): 		214.0380 [0.0356] A 2020yCat.1350....0G
Spectral type is made of 3 parts: %coding is composed of 4 parts :
  • the spectral type, which is made of a temperature class, eventually a luminosity class (roman number) and/or spectral peculiarities;
  • a quality letter: A=best quality→E=worst quality, {� } =unknown quality %
  • a quality letter: A=best quality -> E=worst quality, {� } =unknown quality
  • bibcode : bibcode of the spectral type reference
Spectral type: 		M3.5V C 1983SAAOC...7..106W
Syntax of fluxes (or magnitudes) is : "filter-name (System) flux-value [error] quality MultVarFlags bibcode"
  • filter-name : U, B, V, R, I, G, J, H, K, u, g, r, i, z
  • (System) : may be AB (default is Vega)
  • flux-value : value of flux or magnitude
  • [error] : error value
  • quality : flag of quality of the flux value ( A=best quality -> E=worst quality, {� } =unknown quality)
  • MultVarFlags : Mult is zero or one char (J) for joined photometry ; Var can be zero or two chars (V[0-4])
  • bibcode : bibcode of the flux reference
Fluxes (12) :
U 12.928 [0.0034] B 2009AJ....137.4186L
B 11.749 [0.0017] B 2009AJ....137.4186L
V 10.192 [0.0017] B 2009AJ....137.4186L
R 9.013 [0.0017] B 2009AJ....137.4186L
G 8.875059 [0.002861] C 2020yCat.1350....0G
I 7.462 [0.0017] B 2009AJ....137.4186L
J 5.934 [0.019] C 2003yCat.2246....0C
H 5.349 [0.049] C 2003yCat.2246....0C
K 5.010 [0.021] C 2003yCat.2246....0C
g 10.919 [~] D 2012yCat.1322....0Z
r 9.872 [0.08] D 2012yCat.1322....0Z
i 8.296 [0.05] D 2012yCat.1322....0Z
SIMBAD within arcmin
', {sourceSize:12, color:'#30a090'})); aladin.on('objectClicked', function(object) { var objName=object.data.MAIN_ID; aladin.showPopup(object.ra,object.dec,'',''+ objName+''); });" title="Show Simbad objects"> Overlay Simbad points in this preview
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The search radius has to be specified by the user. It is currently limited to a maximum of 30 arcsec. It depends mostly on the precision or quality of the coordinates (SIMBAD and VizieR catalogs), the resolution of the images from which the sources were extracted, source extent, and source crowding.
Suggestions are: crowded field: 0.5 to 1.5 arcsec, 3 arcsec otherwise; uncertain coordinates (SIMBAD quality E or coordinates without reference): 5 to 30 arsec (risky!). sed-help-icon
Some important notes on this object about identifications and objects associations.
notes:

Hierarchy : number of linked objects
whatever the membership probability is (see description here ) :

: 1
The count displayed here is the number of children objects.
The list obtained by clicking the button may be larger, as some children may be linked with different references or probability.

%This number is the number of distinct objets linked, by using this button, you will obtain all links (may be more than one) from that object to his children

: 4 		: 136 Display criteria :

The link on the acronym of the identifiers give access to the information for this acronym in the dictionary of nomenclature.
Identifiers (42) :
An access of full data is available using the icon Vizier near the identifier of the catalogue

BD-15 6290 HIC 113020 NLTT 55130 UCAC2 26801725
Ci 20 1387 HIP 113020 8pc 212.69A UCAC4 379-165686
EPIC 206019387 JP11 295 PLX 5546 V* IL Aqr
EPIC 206019392 Karmn J22532-142 PLX 5546.00 WEB 20121
GCRV 14365 LFT 1745 PM J22532-1415 WISEA J225317.42-141556.1
GEN# -0.01506290 LHS 530 Ross 780 Zkh 338
G 156-57A LPM 841 TIC 188580272 [RHG95] 3604
G 156-57 LTT 9244 TYC 5819-1255-1 Gaia DR3 2603090003484152064
GJ 876 A 2MASS J22531672-1415489 UBV 19209 Gaia DR2 2603090003484152064
GJ 876 MCC 337 UBV 19610
GSC 05819-00957 NAME NC 59 UBV M 5470

References (1016 between 1850 and 2024) (Total 1016)
Simbad bibliographic survey began in 1850 for stars (at least bright stars) and in 1983 for all other objects (outside the solar system).
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Collections of Measurements


velocities : 9    V* : 5    distance : 3    ROT : 3    Fe_H : 31    PLX : 6    PM : 9    MK : 16   

   

Observing logs


herschel : 3    ISO : 4   

   

External archives :

Link by name to the catalogue in VizieR :

BD-15 6290 G 156-57A G 156-57 GJ 876 A GJ 876
GSC 05819-00957 HIC 113020 HIP 113020 LHS 530 2MASS J22531672-1415489
NLTT 55130 PLX 5546 TYC 5819-1255-1 UCAC2 26801725 UCAC4 379-165686
V* IL Aqr WISEA J225317.42-141556.1 Gaia DR3 2603090003484152064 Gaia DR2 2603090003484152064

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