Lihat sumber bagi Epsilon Eridani

{{Starbox begin
 | name=Epsilon Eridani
}}
{{Starbox image
 | image = 
     <div style="position: relative">[[File:Eridanus IAU.svg|250px|alt=Diagram showing star positions and boundaries of the Eridanus constellation and its surroundings]]
     <div style="position: absolute; left: 49.9%; top: 20.3%">[[File:Cercle rouge 100%.svg|12px]]</div>
     </div>
 | caption = [[Carta bintang]] bagi buruj Eridanus yang menunjukkan kedudukan ε Eridani (dalam bulatan)
}}
{{Starbox observe
 | epoch=[[J2000.0]]
 | constell=[[Eridanus|Eridanus]]
 | ra={{RA|03|32|55.84496}}<ref name=aaa474_2_653/>
 | dec={{DEC|−09|27|29.7312}}<ref name=aaa474_2_653/>
 | appmag_v=3.736<ref name=saaoc8_59/>
}}
{{Starbox character
 | class=K2V<ref name=aj132_1_161/>
 | appmag_1_passband=B
 | appmag_1 =4.61<ref name=SIMBAD/>
 | appmag_2_passband=V
 | appmag_2 =3.73<ref name=SIMBAD/>
 | appmag_3_passband=J
 | appmag_3 ={{nowrap|2.228 ±0.298}}<ref name=cutri2003/>
 | appmag_4_passband=H
 | appmag_4 ={{nowrap|1.880 ± 0.276}}<ref name=cutri2003/>
 | appmag_5_passband=K
 | appmag_5 ={{nowrap|1.776 ± 0.286}}<ref name=cutri2003/>
 | b-v=+0.887<ref name=saaoc8_59/>
 | u-b=+0.571<ref name=saaoc8_59/>
 | variable=[[BY Draconis variable|BY Dra]]<ref name=SIMBAD/><ref name=gcvs/>
}}
{{Starbox astrometry
 | radial_v={{nowrap|+15.5 ± 0.9}}<ref name=rgcrv66/>
 | prop_mo_ra=−975.17<ref name=aaa474_2_653/>
 | prop_mo_dec=19.49<ref name=aaa474_2_653/>
 | parallax=311.37
 | p_error=0.1
 | parallax_footnote=<ref name=aj132_2206/>
 | absmag_v=6.19<ref name=RECONS/>
}}
{{Starbox reference
 | Simbad = HD+22049
 | NSTED =eps+Eridani
 | EPE=eps+Eridani
}}
{{Starbox catalog
 | names = [[Flamsteed designation|18&nbsp;Eridani]], [[Bonner Durchmusterung|BD]]&nbsp;-09°697, [[General Catalogue of Trigonometric Parallaxes|GCTP]]&nbsp;742.00, [[Gliese-Jahreiss catalogue|GJ]]&nbsp;144, [[Henry Draper catalogue|HD]]&nbsp;22049, [[Hipparcos catalogue|HIP]]&nbsp;16537, [[Harvard Revised catalogue|HR]]&nbsp;1084, [[Luyten Half-Second catalogue|LHS]]&nbsp;1557, [[Smithsonian Astrophysical Observatory Star Catalog|SAO]]&nbsp;130564, [[Washington Double Star Catalog|WDS]]&nbsp;03330-0928.<ref name=SIMBAD/>
}}
{{Starbox end}}

'''Epsilon Eridani''' ('''ε Eri''', '''ε Eridani''') ialah sebuah bintang di bahagian selatan buruj [[Eridanus|Eridanus]], pada [[keserongan]] 9.46° selatan [[khatulistiwa samawi]]. Ini membolehkannya dilihat dari kebanyakan tempat di permukaan bumi, pada jarak 10.5 [[tahun cahaya]], ia mempunyai [[magnitud ketara]] 3.73. Ia merupakan bintang individu atau sistem bintang [[Senarai bintang terdekat|ketiga terdekat]] yang membolehkannya dilihat dengan mata kasar dan merupakan bintang yang terdekat yang diketahui mempunyai pelanet sehinggalah penemuan yang tidak disahihkan bagi [[Alpha Centauri Bb]]. Usianya dianggarkan kurang dari satu bilion tahun. Disebabkan usianya yang masih muda, Epsilon Eridani mempunyai [[Medan magnet najam|keaktifan magnet]] yang tinggi berbanding Matahari masa kini, dengan [[angin najam]] sekuat 30 kali ganda. Tempoh putarannya ialah 11.2&nbsp;hari di khatulistiwanya. Epsilon Eridani adalah lebih kecil dan kurang berjisim berbanding Matahari, dan secara bandingannya mempunyai sedikit [[kelogaman|unsur yang lebih berat daripada helium]].<ref name="aaa426"/> Ia merupakan bintang [[jujukan utama]] bagi [[kelas spektrum]] K2, yang bemaksud tenaganya dijana di teras melalui [[pelakuran nuklear]] [[hidrogen]] yang dipancarkan ke permukaan pada suhu lebih kurang 5,000&nbsp;[[Kelvin|K]], yang memberikannya warna kejinggaan.

Pergerakan Epsilon Eridani sepanjang garis penglihatan dari Bumi, dikenali sebagai [[halaju jejarian]], sering dicerap lebih daripada dua puluh tahun. Perubahan berkalanya memberikan bukti tentang kewujudan [[planet gergasi]] mengelilingi Epsilon Eridani, menjadikannya satu daripada sistem luar suria dengan calon planet yang terhampir.<ref name=apj544_2_L145/> Objek tersebut, [[Epsilon Eridani b]], secara rasminya diumumkan pada tahun 2000 oleh sepasukan ahli astronomi yang diketuai oleh Artie Hatzes.<ref name=apj544_2_L145/> Data terkini menunjukkan yang planet ini mengelilingi bintangnya dalam tempoh 7 tahun dengan pemisahan purata 3.4 [[unit astronomi]] (AU), 1&nbsp;AU pula bersamaan jarak purata antara Bumi dan Matahari.<ref name=eep_eps_eri/> Walaupun peneman ini berkontroversi disebabkan jumlah hingar latar belakang bagi data halaju jejariannya yang tinggi,<ref name=asp2003/> banyak ahli astronomi menganggap kewujudan planet tersebut sebagai sahih.

Sistem tersebut termasuklah dua gegelung batuan [[asteroid]]: satu pada 3&nbsp;AU dan yang kedua pada kedudukan lebih kurang 20&nbsp;AU, yang strukturnya dipelihara oleh planet hipotesis kedua, Epsilon Eridani c.<ref name=aguilar_pulliam20081027/> Epsilon Eridani turut mempunyai [[cakera puing]] luaran bagi sisa planetesimal hasil baki semasa pembentukan sistem tersebut.<ref name=apj690_2_1522 />

Penamaan Epsilon Eridani diasaskan pada tahun 1603 oleh [[Johann Bayer]]. Ia berkemungkinan sebahagian daripada bintang Kumpulan Bergerak Ursa Major yang berkongsi pergerakan serupa merentasi [[Bima Sakti]], menunjukkan yang bintang ini berkongsi asal usul ari sebuah [[kelompok terbuka]]. Jiran terdekatnya, sistem bintang deduaan [[Luyten 726-8]], akan berada pada kedudukan paling hampir dengan Epsilon Eridani dalam lebih kurang 31,500&nbsp;tahun yang ketika itu hanya dipisahkan lebih kurang 0.93&nbsp;ly.<ref name=potemine10/> Sebagai bintang menyerupai Matahari yang terhampir dengan potensi untuk mempunyai hidupan,<ref name=villard35_12_44/> Epsilon Eridani telah menjadi sasaran dalam pencarian [[SETI]]. Epsilon Eridani muncul dalam kisah cereka sains dan dicadangkan sebagai destinasi penjelajahan antarnajam.<ref name=boyle2009/> Dari Epsilon Eridani, Matahari akan kelihatan sebagai sebuah bintang dengan magnitud 2.4 di [[Serpens]].<ref name=sun group=note/>

== Sejarah pencerapan ==
[[File:Epsilon Eridani location.png|right|thumb|Atas, bahagian utara buruj Eridanus ditandakan dengan hijau, manakala garisan biru menunjukkan [[Buruj Orion|Orion]]. Bawah, pandangan yang diperbesarkan dalam kotak putih menunjukkan Epsilon Eridani di persimpangan dua garis.|alt=Gambar atas menunjukkan kawasan bintang dengan garisan warna menunjukkan buruj. Gambar bawah menunjukkan beberapa bintang dengan dua garis putih.]]

=== Pengkatalogan ===

===Pengesana penghampiran===
Berdasarkan pemerhatian antara 1800 dan 1880, Epsilon Eridani didapati mempunyai gerakan benar yang besar merentasi [[sfera samawi]], yang dianggarkan pada [[halaju sudut]] tiga [[arkasaat]] setiap tahun. <ref name=mras48_77/> Gerakan ini menunjukkan ia agak dekat dengan Matahari,<ref name=belkora2002/> menjadikannya bintang tumpuan bagi tujuan pengukuran [[paralaks]] trigonometri . Proses ini melibatkan rakaman kedudukan Epsilon Eridani semasa Bumi bergerak mengelilingi Matahari, yang membolehkan jarak bintang dianggar. <ref name=mras48_77/> Dari 1881-1883, ahli astronomi Amerika William L. Elkin menggunakan [[heliometer]] di [[Balai Cerap Diraja Tanjung Harapan]], [[Afrika Selatan]] untuk membandingkan kedudukan Epsilon Eridani dengan dua bintang yang berdekatan. Dari pemerhatian ini, pengukuran paralaks {{nowrap | 0.14 ± 0.02 arkasaat}} telah dikira <ref name=gill1893/> <ref name=gill1884 />. Menjelang 1917, pemerhati telah memperbaiki anggaran paralaks mereka kepada 0.317 arkasaat.<ref name=apj46_313/> Nilai moden bagi 0.3109 arkasaat adalah bersamaan dengan jarak kira-kira {{convert|10.50|ly|pc|abbr=in}}.<ref name=aaa474_2_653/>

===Penemuan keliling najam===

===Catatan===
{{reflist|colwidth=50em|group=note|refs=

{{refn|1=From Epsilon Eridani, the Sun would appear on the diametrically opposite side of the sky at the coordinates RA={{RA|15|32|55.84496}}, Dec={{DEC|09|27|29.7312}}, which is located near [[Alpha Serpentis]]. The absolute magnitude of the Sun is 4.83,<sup>[a]</sup> so, at a distance of 3.212&nbsp;parsecs, the Sun would have an apparent magnitude:
<math>\begin{smallmatrix} m = M_v + 5\cdot\log_{10} (3.212/10) + A_V = 2.36 \end{smallmatrix}</math>,<sup>[b]</sup> assuming negligible [[Extinction (astronomy)|extinction]] (A<sub>V</sub>) for a nearby star.
<br>Ref.:
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===Rujukan===
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== Pautan luar ==
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*{{citation | author=Staff | title=Astronomers discover a nearby star system just like our own Solar System | date=July 8, 1998 | work=Joint Astronomy Centre | publisher=The University of Hawaii | url=http://outreach.jach.hawaii.edu/pressroom/1998_epseri/ | accessdate=2011-02-24 | postscript=. }}
*{{citation | author=Anonymous | title=Epsilon Eridani | work=SolStation | publisher=The Sol Company | url=http://www.solstation.com/stars/eps-erid.htm | accessdate=2008-11-28 | postscript=. }}
*{{citation | first1=Wil | last1=Tirion | title=Sky Map: Epsilon Eridani | publisher=Cambridge University Press | publication-place=Cambridge, U.K. | year=2001 | work=Planet Quest | url=http://planetquest1.jpl.nasa.gov/atlas/atlas_skymap.cfm?Planet=109&Zoom=1 | accessdate=2011-04-09 | postscript=. | archive-date=2011-07-26 | archive-url=https://web.archive.org/web/20110726151258/http://planetquest1.jpl.nasa.gov/atlas/atlas_skymap.cfm?Planet=109&Zoom=1 | url-status=dead }}