Vicsek fractal: Difference between revisions
Jump to navigation
Jump to search
en>Mild Bill Hiccup m →Properties: spelling |
en>AnonMoos natural size |
||
| Line 1: | Line 1: | ||
{{Planetbox begin | |||
| name = [[Harvard Revised catalogue|HR]] 8799 d | |||
}} | |||
{{Planetbox image | |||
| image = Exoplanet Comparison HR 8799 d.png | |||
| caption = Size comparison of HR 8799 d (gray) with Jupiter. | |||
}} | |||
{{Planetbox star | |||
| star = [[HR 8799]] | |||
| constell = [[Pegasus (constellation)|Pegasus]] | |||
| RA = {{RA|23|07|28.7150}}<ref name="SIMBAD">{{SIMBAD link|HR+8799|V* V342 Peg -- Variable Star of gamma Dor type}}, entry, [[SIMBAD]]. Accessed on line November 14, 2008.</ref> | |||
| DEC = {{DEC|+21|08|03.302}}<ref name="SIMBAD" /> | |||
| app_mag = 5.964<ref name="SIMBAD" /> | |||
| dist_ly = 129 ± 4<ref name="vanLeeuwen2007">{{cite web|url=http://webviz.u-strasbg.fr/viz-bin/VizieR-5?-out.add=.&-source=I/311/hip2&recno=113804|title=HIP 114189|work=Hipparcos, the New Reduction|author=van Leeuwen, F.|year=2007|accessdate=2008-10-13}}</ref><ref group="note" name="calculate_distance">Computed from parallax: <math>\scriptstyle \mathrm{distance\ in\ parsecs}=\frac{1000}{\mathrm{parallax\ in\ milliarcseconds}}</math></ref> | |||
| dist_pc = 39 ± 1<ref name="vanLeeuwen2007" /><ref group="note" name="calculate_distance" /> | |||
| class = kA5 hF0 mA5 V; λ Boo<ref name="Gray1999">{{cite journal|title=HR 8799: A Link between γ Doradus Variables and λ Bootis Stars|author=Gray, R.O. and Kaye, A.B.|year=1999|journal=[[The Astronomical Journal]]|volume=118|issue=6|pages=2993–2996|doi=10.1086/301134|bibcode=1999AJ....118.2993G}}</ref><ref name="Kaye1999">{{cite journal|title=Gamma Doradus Stars: Defining a New Class of Pulsating Variables|author=Kaye, A.B. ''et al.''|year=1999|journal=[[PASP]]|volume=111|issue=761|pages=840–844|bibcode=1999PASP..111..840K|doi=10.1086/316399|arxiv = astro-ph/9905042 }}</ref> | |||
}} | |||
{{Planetbox separation | |||
| epoch = 2008-09-18 | |||
| separation_mas = 621<ref name="Marois2008">{{cite journal |last=Marois |first=Christian |authorlink= |coauthors=''et al.'' |date=November 2008 |title=Direct Imaging of Multiple Planets Orbiting the Star HR 8799 |journal=[[Science (journal)|Science]] |volume=322 |issue=5906 |pages=1348–1352 |doi=10.1126/science.1166585 |arxiv=0811.2606 |accessdate= |quote= |pmid=19008415 |bibcode = 2008Sci...322.1348M }}</ref><ref group="note" name="separation">Calculated from the separations in the East and North directions which are −0.216 and −0.582 [[arcsecond]]s respectively.</ref> | |||
| position_angle = 200.36<ref name="Marois2008" /><ref group="note" name="separation" /> | |||
| separation = 24<ref name="Marois2008" /> | |||
}} | |||
{{Planetbox orbit | |||
| semimajor = ~24<ref name="Marois2008" /><ref group="note" name="circular_orbit">Value given assuming the planet's orbit is circular and is being observed face-on.</ref> | |||
| semimajor_gm = ~3600 | |||
| eccentricity = >0.04<ref>{{cite journal |title=Stability of the directly imaged multiplanet system HR 8799: resonance and masses |author=Fabrycky ''et al.'' |date=1 December 2008|pages=1408–1421 |accessdate=2008-12-02 |issue=2 |volume=710 |author2=Murray-Clay |doi=10.1088/0004-637X/710/2/1408 |journal=Astrophys.J. |arxiv=0812.0011|bibcode = 2010ApJ...710.1408F }}</ref><ref group="note">The lower limit on the eccentricity is given for the case that the planet is in a 2:1 resonance with [[HR 8799 c]], as suggested by stability constraints.</ref> | |||
| period_year = ~100<ref name="Marois2008" /><ref group="note" name="circular_orbit" /> | |||
}} | |||
{{Planetbox character | |||
| mass = 7{{±|3|2}}<ref>{{cite arxiv |eprint=1011.4918 |author1=Marois |author2=Zuckerman |author3=Konopacky |author4=Macintosh |author5=Barman |title=Images of a fourth planet orbiting HR 8799 |class=astro-ph.EP |year=2010}}</ref> | |||
| radius = 1.2{{±|0.1|0}}<ref name="Marois2008" /> | |||
| density = 4{{±|1.75|1.1}} | |||
| temperature = 1090{{±|10|90}}<ref name="Marois2008" /> | |||
}} | |||
{{Planetbox discovery | |||
| discovery_date = November 13, 2008 | |||
| discoverers = Marois ''et al.'' | |||
| discovery_method = [[Direct imaging]] | |||
| discovery_site = [[W.M. Keck Observatory|Keck]] and [[Gemini Observatory|Gemini<br/>observatories]] in [[Hawaii]] | |||
| discovery_status = Published | |||
}} | |||
{{Planetbox catalog | |||
| names = [[Henry Draper catalogue|HD]] 218396 d<ref>{{SIMBAD link|HD+218396d|HD 218396d -- Extra-solar Planet Candidate}}, entry, [[SIMBAD]]. Accessed on line December 6, 2008.</ref> | |||
}} | |||
{{Planetbox reference | |||
| star = HR+8799 | |||
| planet = d | |||
| simbad = HD+218396d | |||
}} | |||
{{Planetbox end}} | |||
'''HR 8799 d''' is an [[extrasolar planet]] located approximately 129 [[light-year]]s away in the [[constellation]] of [[Pegasus (constellation)|Pegasus]], orbiting the 6th [[apparent magnitude|magnitude]] [[Lambda Boötis star]] [[HR 8799]]. It has a mass between 5 and 10 [[Jupiter mass]]es and a radius from 20 to 30% larger than [[Jupiter]]'s. The planet orbits at 24 [[astronomical units|AU]] from HR 8799 with an eccentricity greater than 0.04 and a period of 100 years. Upon initial discovery, it was the innermost known planet in the HR 8799 system, but '''[[HR 8799 e|e]]''', discovered later, is now known to be closer to their parent star. Along with two other planets orbiting HR 8799, this planet was discovered on November 13, 2008 by Marois ''et al.'', using the [[W.M. Keck Observatory|Keck]] and [[Gemini Observatory|Gemini observatories]] in [[Hawaii]]. These planets were discovered using the [[direct imaging]] technique.<ref name="Marois2008" /><ref>{{cite press release|url=http://www.keckobservatory.org/article.php?id=231|title=Astronomers capture first images of newly-discovered solar system|publisher=W. M. Keck Observatory|date=2008-11-13|accessdate=2008-12-02}}</ref><ref>{{cite press release|url=http://www.gemini.edu/node/11151|title=Gemini Releases Historic Discovery Image of Planetary First Family|publisher=Gemini Observatory|date=2008-11-13|accessdate=2008-12-02}}</ref><ref>{{cite news|title=Scientists Publish First Direct Images of Extrasolar Planets|first=Joel|last=Achenbach|work=[[The Washington Post]]|publisher=[[The Washington Post Company]]|date=2008-11-13|accessdate=2008-12-02|url=http://www.washingtonpost.com/wp-dyn/content/article/2008/11/13/AR2008111302267.html}}</ref> | |||
Near infrared spectroscopy from 995 to 1769 nanometers made with the Palomar Obervatory show evidence of Acetylene, Methane, and Carbon Dioxide, but Ammonia is not definitively detected.<ref name=Gilliland>{{cite web|first = B. R. Oppenheimer|title= Reconnaissance of the HR 8799 Exosolar System I: Near IR Spectroscopy|url=http://arxiv.org/abs/1303.2627|publisher=Cornell University|accessdate=12 March 2013}}</ref> | |||
__NOTOC__ | |||
==Notes== | |||
<references group="note" /> | |||
==See also== | |||
* [[Fomalhaut b]] | |||
==References== | |||
{{reflist}} | |||
==External links== | |||
{{Commons category-inline}} | |||
* {{cite web | url=http://media4.obspm.fr/exoplanets/base/planete.php?etoile=HR+8799&planete=d | title=HR 8799 d | work=Exoplanets}} | |||
{{HR 8799}} | |||
{{Sky|23|07|28.7150|+|21|08|03.302|129}} | |||
{{DEFAULTSORT:Hr 8799 D}} | |||
[[Category:HR 8799]] | |||
[[Category:Exoplanets discovered in 2008]] | |||
[[Category:Gas giants]] | |||
[[Category:Pegasus (constellation)]] | |||
[[Category:Exoplanets detected by direct imaging]] | |||
{{extrasolar-planet-stub}} | |||
Latest revision as of 17:43, 16 May 2013
Template:Planetbox begin Template:Planetbox image Template:Planetbox star Template:Planetbox separation Template:Planetbox orbit Template:Planetbox character Template:Planetbox discovery Template:Planetbox catalog Template:Planetbox reference Template:Planetbox end
HR 8799 d is an extrasolar planet located approximately 129 light-years away in the constellation of Pegasus, orbiting the 6th magnitude Lambda Boötis star HR 8799. It has a mass between 5 and 10 Jupiter masses and a radius from 20 to 30% larger than Jupiter's. The planet orbits at 24 AU from HR 8799 with an eccentricity greater than 0.04 and a period of 100 years. Upon initial discovery, it was the innermost known planet in the HR 8799 system, but e, discovered later, is now known to be closer to their parent star. Along with two other planets orbiting HR 8799, this planet was discovered on November 13, 2008 by Marois et al., using the Keck and Gemini observatories in Hawaii. These planets were discovered using the direct imaging technique.[1][2][3][4]
Near infrared spectroscopy from 995 to 1769 nanometers made with the Palomar Obervatory show evidence of Acetylene, Methane, and Carbon Dioxide, but Ammonia is not definitively detected.[5]
Notes
See also
References
43 year old Petroleum Engineer Harry from Deep River, usually spends time with hobbies and interests like renting movies, property developers in singapore new condominium and vehicle racing. Constantly enjoys going to destinations like Camino Real de Tierra Adentro.
External links
Template:Commons category-inline
Template:Extrasolar-planet-stub
- ↑ Cite error: Invalid
<ref>tag; no text was provided for refs named "Marois2008". - ↑ Template:Cite press release
- ↑ Template:Cite press release
- ↑ Template:Cite news
- ↑ Template:Cite web