Kepler-46

{{Starbox image

| image = 250px

| caption = Artist's conception of the Kepler-46 system showing the two planets. Planet b transits its star, the same method by which it was detected.

}}

{{Starbox observe

| epoch = J2000

| constell = Lyra

| ra = {{RA|19|17|04.4930}}

| dec = {{DEC|42|36|15.041}}

| appmag_v =

}}

{{Starbox character

| class =

| appmag_1_passband =

| appmag_1 =

| appmag_2_passband =

| appmag_2 =

| appmag_3_passband = J

| appmag_3 = 13.814{{cite simbad | title=Kepler-46 | access-date=May 16, 2012}}

| appmag_4_passband = H

| appmag_4 = 13.436

| appmag_5_passband = K

| appmag_5 = 13.347

| r-i =

| v-r =

| b-v =

| u-b =

| variable =

}}

{{Starbox astrometry

| radial_v =

| prop_mo_ra = {{val|3.101|(24)}}

| prop_mo_dec = {{val|0.864|(27)}}

| pm_footnote =

| parallax = 1.2963

| p_error = 0.0225

| parallax_footnote =

| absmag_bol = 5.18 (predicted)Figure based on the following equations, which calculated bolometric (total) luminosity across all spectra based on effective temperature: $m_{\rm star}=m_{\rm sun}-2.5\log_{10}\left({ L_{\rm star} \over L_{\odot} } \cdot \left(\frac{ d_{\rm sun} }{ d_{\rm star} }\right)^2\right)$ (cf. Luminosity) and $M = m_{\rm star} - 5 ((\log_{10}{D_L}) - 1)\!\,$ (cf. Absolute magnitude)

}}

{{Starbox detail

| mass = {{val|0.902|0.040|0.038}}

| radius = {{val|0.938|0.038|0.039}}

| luminosity_bolomatric = 0.868 ± 0.155 (predicted)The equation used to calculate this was : $\frac{L}{L_{\odot}} = {\left ( \frac{R}{R_{\odot}} \right )}^2 {\left ( \frac{T}{T_{\odot}} \right )}^4$ .

| temperature = {{val|5155|150}}

| metal_fe = {{val|0.41|0.10}}This measurement indicates the log₁₀ of the relative abundance of iron in the measured star to that of the Sun.

| rotation = {{val|27.859|0.075|s= days}}

| age_gyr = {{val|9.7|3.7|3.5}}

}}

{{Starbox catalog

| names = {{odlist | 2MASS=J19170449+4236150 | Gaia DR2=2102700131386216576 | KIC=7109675 | KOI=872 }}

}}

{{Starbox reference

| Simbad = Kepler-46

| KIC = 7109675

}}

Kepler-46, previously designated KOI-872, is a star located in the constellation Lyra. Observed since 2009 by the Kepler space observatory, it has since been found to possess a planetary system consisting of at least three planets and while it has a similar mass to the Sun (90%) it is significantly older at ten billion years.

Kepler-46 b (previously KOI-872.01), was the first planet discovered in the system. It was found through detailed analysis of Kepler space observatory data. An additional planet, Kepler-46 c, was discovered by an outside group using Kepler public data through analysis of transit timing variations. While only one additional planet was confirmed by the analysis, the study revealed the potential existence of an unconfirmed planet KOI-872.03 (KOI-872 d). Validation by the multiplicity method confirmed the existence of this planet which was then renamed Kepler-46d.

Planetary system

Planet b is a gas giant planet with a mass slightly less than that of Jupiter. The second planet in the system was among the first to be discovered through the method of transit timing variations, and through its confirmation of KOI-872 c with a 99% confidence level has shown that the method of detection may be used to detect future extrasolar planets and, possibly, extrasolar moons.{{cite news | url=http://www.space.com/15631-hidden-alien-planet-gravity-discovery.html | title=Hidden Alien Planet Revealed by Its Own Gravity| work=Space.com | date=May 10, 2012 | agency=Space.com | access-date=May 10, 2012 | author=Moskowitz, Clara}} This second planet exerted a gravitational force on the first planet, orbiting its host star in just 34 days. While this usually occurs on an extremely regular schedule, additional planets within the system can disrupt the time of the transit, and these disruptions can indicate the presence of a planet, even if the disrupting planet does not pass in front of the host star itself.

The data show that Kepler-46 c is an approximately Saturn-mass object with an orbital period of 57 days. As the planet does not itself transit its host star, there is no way of knowing its size (probably a similar size to its sibling). The measurements also suggest the existence of another planet orbiting with a period of about 6.8 days, and this planet was confirmed in 2016.{{citation|arxiv=1601.05095|year=2016|title=Warm Jupiters Are Less Lonely Than Hot Jupiters: Close Neighbors|doi=10.3847/0004-637X/825/2/98|last1=Huang|first1=Chelsea|last2=Wu|first2=Yanqin|author2-link= Yanqin Wu |last3=Triaud|first3=Amaury H. M. J.|journal=The Astrophysical Journal|volume=825|issue=2|page=98|bibcode=2016ApJ...825...98H|s2cid=119290761 |doi-access=free }}

The method in which the planet was detected is similar to the way that the planet Neptune was discovered, in which the newly discovered planet is detected by its pull on another which is already known to exist.{{cite news | url=http://earthsky.org/space/new-planet-found-in-distant-solar-system-by-its-tug-on-another-world | title=New planet found in distant solar system by its tug on another world | work=EarthSky | date=May 12, 2012 | agency=Earthsky Communications | access-date=May 19, 2012 | author=Crockett, Christopher}}

In 2021, it was found the orbital plane of Kepler-46b is slowly changing, likely under the gravitational influence of the additional giant planet.{{citation|arxiv=2105.04318|year=2021|title=Systematic search for long-term transit duration changes in Kepler transiting planets|doi=10.1093/mnras/stab1359 |last1=Shahaf |first1=Sahar |last2=Mazeh |first2=Tsevi |last3=Zucker |first3=Shay |last4=Fabrycky |first4=Daniel |journal=Monthly Notices of the Royal Astronomical Society |volume=505 |issue=1 |pages=1293–1310 |doi-access=free |bibcode=2021MNRAS.505.1293S }}

{{Orbitbox planet begin

| table_ref =

}}

{{OrbitboxPlanet

| exoplanet = d

| semimajor = {{val|0.0679|0.0035}}

| period = {{val|6.76671|0.00013|0.00012}}

| eccentricity = 0(assumed)

| inclination = {{val|88.55|0.49|0.69}}

| radius = {{val|0.1510|0.0094|0.0098}}

|mass_earth={{val|3.339|}}}}

{{OrbitboxPlanet

| exoplanet = b

| mass = {{val|0.885|0.374|0.343}}

| semimajor = {{val|0.1971|0.0001}}

| period = {{val|33.648|0.004|0.005}}

| eccentricity = {{val|0.0321|0.0069|0.0078}}

| inclination = {{val|89.04|0.14}}

| radius = {{val|0.810|0.035|0.36}}

}}

{{OrbitboxPlanet

| exoplanet = c

| mass = {{val|0.362|0.016}}

| semimajor = {{val|0.2811|0.0003}}

| period = {{val|57.325|0.116|0.098}}

| eccentricity = {{val|0.0354|0.0057|0.0059}}

| inclination = {{val|88.66|0.26|0.27}}

}}

References

{{reflist|refs=

{{cite journal | title=Stellar Rotation Periods of The Kepler objects of Interest: A Dearth of Close-In Planets Around Fast Rotators | last1=McQuillan | first1=A. | last2=Mazeh | first2=T. | last3=Aigrain | first3=S. | journal=The Astrophysical Journal Letters | volume=775 | issue=1 | at=L11 | year=2013 | arxiv=1308.1845 | bibcode=2013ApJ...775L..11M | doi=10.1088/2041-8205/775/1/L11 | s2cid=118557681 }}

{{cite journal | title=The Detection and Characterization of a Nontransiting Planet by Transit Timing Variations | last1=Nesvorny | first1=D. | last2=Kipping | first2=D. M. | last3=Buchhave | first3=L. A. | last4=Bakos | first4=G. A. | last5=Hartman | first5=J. | last6=Schmitt | first6=A. R. | display-authors=1 | journal=Science | volume=336 | issue=6085 | pages=1133–6 | year=2012 | arxiv=1208.0942 | bibcode=2012Sci...336.1133N | doi=10.1126/science.1221141 | pmid=22582018 | s2cid=41455466 }}

{{cite journal | title=Masses of Kepler-46b, c from Transit Timing Variations | last1=Saad-Olivera | first1=Ximena | last2=Nesvorný | first2=David | last3=Kipping | first3=David M. | last4=Roig | first4=Fernando | display-authors=1 | journal=The Astronomical Journal | volume=153 | issue=4 | at=198 | year=2017 | arxiv=1704.01541 | bibcode=2017AJ....153..198S | doi=10.3847/1538-3881/aa64e0 | s2cid=119513521 | doi-access=free }}

}}

Notes

Category:Lyra

Category:Planetary systems with three confirmed planets

872

Category:Planetary transit variables