海王星
航行者2號影到嘅海王星 | |||||||||||||||||||||
發現 | |||||||||||||||||||||
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發現人 | 埃班勒維耶 約翰伽雷 | ||||||||||||||||||||
發現日子 | 1846年9月23號[1] | ||||||||||||||||||||
軌道參數[3][4] | |||||||||||||||||||||
曆元 J2000 | |||||||||||||||||||||
遠日點 | 4,553,946,490 km 30.44125206 AU | ||||||||||||||||||||
近日點 | 4,452,940,833 km 29.76607095 AU | ||||||||||||||||||||
半長軸 | 4,503,443,661 km 30.10366151 AU | ||||||||||||||||||||
離心率 | 0.011214269 | ||||||||||||||||||||
軌道週期 | 60,327.624日 165.17156年 | ||||||||||||||||||||
會合週期 | 367.49 day[2] | ||||||||||||||||||||
平均速度 | 5.43 km/s[2] | ||||||||||||||||||||
平近點角 | 267.767281° | ||||||||||||||||||||
軌道傾角 | 1.767975° 6.43° 對太陽嘅赤道 | ||||||||||||||||||||
升交點黃經 | 131.794310° | ||||||||||||||||||||
近日點參數 | 265.646853° | ||||||||||||||||||||
衛星 | 16 | ||||||||||||||||||||
物理特徵 | |||||||||||||||||||||
赤道半徑 | 24,764±15 km[5][6] 3.883 Earths | ||||||||||||||||||||
極半徑 | 24,341±30 km[5][6] 3.829 Earths | ||||||||||||||||||||
表面積 | 7.6408×109 km²[6][7] 14.94 Earths | ||||||||||||||||||||
體積 | 6.254×1013 km³[2][6] 57.74 Earths | ||||||||||||||||||||
質量 | 1.0243×1026 kg[2] 17.147 Earths | ||||||||||||||||||||
平均密度 | 1.638 g/cm³[2][6] | ||||||||||||||||||||
表面重力 | 11.15 m/s²[2][6] 1.14 g) | ||||||||||||||||||||
逃逸速度 | 23.5 km/s[2][6] | ||||||||||||||||||||
恒星自轉週期 | 0.6 day[2] 15 h 57 min 59 s | ||||||||||||||||||||
赤道自轉速度 | 2.68 km/s 9,660 km/h | ||||||||||||||||||||
轉軸傾角 | 28.32°[2] | ||||||||||||||||||||
北極赤經 | 17 h 19 min 59 s 299.333°[5] | ||||||||||||||||||||
北極赤緯 | 42.950°[5] | ||||||||||||||||||||
反照率 | 0.290 (bond) 0.41 (geom.)[2] | ||||||||||||||||||||
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視星等 | 8.0 to 7.78 [2] | ||||||||||||||||||||
角直徑 | 2.2" — 2.4" [2] | ||||||||||||||||||||
大氣[2] | |||||||||||||||||||||
大氣標高 | 19.7±0.6 km | ||||||||||||||||||||
成分 |
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海王星(粵拼:hoi2 wong4 sing1;英文:Neptune;拉丁文:Neptunus)係太陽系其中一粒行星,距離太陽第八近,亦都係離太陽最遠嗰粒行星。要留意嘅係,有時因為矮行星冥王星軌道離心率高,位置會入過海王星軌道,所以有時冥王星距離太陽仲近過海王星[8]。
海王星算係太陽系入面比較大嘅行星:以行星直徑嚟講,海王星喺太陽系排第四,而質量佢就排第三,僅次於土星同木星-佢嘅質量係地球嘅 17.147 倍,而孖生兄弟天王星就得地球嘅14.536倍,噉係因為天王星嘅密度明顯低啲;目前海王星有14粒衛星[9],而且佢仲有個唔多光(所以唔容易睇到)嘅行星環[9]。
天文學家有深入噉研究過海王星嘅大氣層:海王星嘅大氣層主要由氫同氦組成;佢仲含有少量嘅甲烷,令佢睇起嚟係淺藍色嘅,不過海王星嘅藍色色調比天王星嘅多[10];海王星亦擁有太陽系中所有行星中最強嘅風,高達時速2,100公里,即係時速1,300英里[11];有一次,天文學家喺海王星北半球發現咗一個大黑斑(好似木星表面嘅「大紅斑」風暴咁),但唔知點解,過咗幾年個大黑斑走咗去南半球[12]。
歷史
[編輯]發現
[編輯]伽利略喺1612年2月28號首次觀測到海王星,而喺1613年1月27號,佢再次觀測海王星,但因為佢喺夜空中同木星好近,所以伽利略並冇發現佢係一粒行星,而覺得佢係一粒恆星[13]。喺佢第一次觀測入面,海王星啱啱開始逆行,而郁動好細,導致伽利略嘅細望遠鏡未能發現倒[14]。喺2009年一項研究話伽利略至少意識到佢睇倒嘅「恆星」有好細嘅郁動[15]。
1821年,Alexis Bouvard 發表咗天王星軌道嘅天文表[16],但之後嘅觀察發現天王星嘅軌道同張表有好大偏差,令Alexis Bouvard 假設有未知物體干擾軌道[17]。1843年,John Couch Adams 利用佢掌握嘅數據開始研究天王星嘅軌道。佢要求皇家天文學家George Airy爵士提供額外數據,Airy喺1844年2月提供咗呢啲數據。Adams喺1845至46年繼續研究,並估計咗一粒新行星係點[18][19]。
1845-46年勒維耶獨立喺Adams,發展咗自己嘅計算方法,但未引起同好熱情。1846年6月,喺睇到勒維耶對行星經度嘅估計同Adams嘅估計好似之後,Airy說服咗James Challis揾呢粒行星。Challis喺1846年8-9月持續噉揾呢粒行星[17][20]。
此時,勒維耶亦都揾咗柏林天文台嘅約翰伽雷幫手揾行星,柏林天文臺嘅學生達赫斯特話可以用勒維耶預測位置區域嘅天空圖同嗰陣嘅天空比較。喺1846年9月23號夜晚,伽雷就發現咗海王星,喺同勒維耶預測嘅位置差1度[21][22],同Adams預測嘅位置差12度。之後,Challis發現佢喺8月嗰陣已經睇倒海王星兩次,但因為唔重視揾海王星嘅任務,未進行分析就承認呢啲觀察結果。Challis好後悔,但將佢嘅疏忽歸咎於佢過時嘅星圖同分心嘅事實[17][23][24]。
命名
[編輯]喺佢被發現之後冇耐,啲人叫佢「天王星外面嘅行星」、「勒維耶嘅行星」。伽雷提出咗第一個名嘅提議,叫Janus,而喺英國,Challis提議話佢叫Oceanus[25]。
勒維耶聲稱佢有權為行星命名,幫粒行星改咗個名做Neptune,但錯誤噉話已經得到法國經度局批准[26]。10月,佢想用自己個名Le Verrier命名行星,並得到天文台台長Fran ois Arago嘅支持。呢項提議喺法國以外被強烈反對[27]。法國曆書好快將天王星命名做天王星嘅發現者赫歇爾,並用勒維耶個名叫呢個新行星[28]。之後,勒維耶經由經度委員會提議用Neptune做呢粒行星個名。腓特烈·斯特魯維喺1846年12月29號喺聖彼得堡支持勒維耶嘅提議[29],好快Neptune就做咗國際公認嘅呢粒新行星嘅名。喺羅馬神話入面,Neptune係海神,同希臘嘅海神波塞冬一樣,所有呢啲行星都以羅馬或希臘神話入面嘅神來命名[30]。而其他文都用海神嘅名來叫呢粒行星,例如中文,越南文,日文同韓文入面嘅海王星[31][32]。
狀況
[編輯]喺1846年發現海王星之後,海王星係當時已知行星當中最遠嘅,直到1930年又發現有冥王星;嗰陣啲人認為冥王星係一粒行星,所以海王星就成為咗已知行星當中第二遠嘅[33]。1992年發現咗柯伊伯帶件事導致好多天文學家開始爭詏係應該當冥王星係行星抑或係柯伊伯帶嘅一部分[34]。到2006年,國際天文學聯合會首次定義「矮行星」,並劃冥王星成矮行星,令到海王星變返太陽系入邊最外圍粒行星[35]。
物理同化學性質
[編輯]海王星嘅質量係1.0243×1026公斤[2],係地球17倍,木星嘅十九分之一。佢喺1巴嗰陣嘅引力係11.15 m/s²,係地球表面引力嘅1.14倍[36],只係細過木星[37]。
海王星赤道半徑係24,764公里[38],差唔多係地球四倍。海王星同天王星一樣,係冰巨行星,同氣體大行星唔同,比氣體大行星細,成份亦同佢哋有啲唔同[39]。
內部結構
[編輯]海王星內部結構同天王星差唔多。大氣層佔佢質量5-10%,並可能向核心延伸咗10-20%,喺嗰度壓力有大約10GPa,大概係地球壓力嘅100,000倍。喺大氣層較低區域有比上層更多嘅甲烷、氨同水[40]。
地幔有成10-15個地球質量,有更加多氨、水同甲烷[41]。照行星科學慣例,呢樣嘢被人叫做冰,佢係一種熱嘅流體,通常被人叫做水-氨大洋[42]。
喺地底下7000公里,可能有甲烷分解做鑽石晶體,然後好似落雨噉跌落[43][44][45],噉樣被人叫做鑽石雨。科學家仲覺得呢個現象喺木星、土星同天王星上面都有發生[46]。
海王星嘅核心可能由鐵、鎳同矽酸鹽組成,內核質量大概係地球嘅1.2倍[47]。中心嘅壓力係7Mbar(700GPa),大約係地球中心嘅兩倍,溫度可能係5,400K[40][48]。
大氣層
[編輯]喺高海拔地區,大氣層有80%嘅氫同19%嘅氦[40],亦有少量甲烷。吸收帶喺600納米以上嘅波長,喺光譜紅色至紅外線一帶。噉嘅吸收令海王星呈現淺藍色,同天王星一樣[49],而天王星睇落隻色比較淺,因為天王星大氣入面嘅霧霾更加濃[50]。
海王星嘅大氣層被人分做兩個區域,一個係對流層低層,海拔越高溫度越低;另一個係平流層,海拔越高溫度越高。兩個區嘅邊界,壓力有0.1巴[51]。平流層喺1-10帕斯卡度成為熱成層[51],然後逐漸過渡去散逸層。
模型表明海王星嘅對流層雲帶由唔同成分組成,並取決於海拔高度[52]。上層雲層壓力低過1bar,溫度適合甲烷凝結。壓力1至5bar嘅地方被認為會形成氨同硫化氫雲。而壓力高過5bar嗰陣,雲可能由氨、硫化銨、硫化氫同水組成。喺大約50bar嘅壓力之下,溫度達到0 °C嗰陣,可能會有更加深嘅水冰雲。喺下面啲嘅地方可能會發現氨同硫化氫嘅雲[53]。
海王星上面嘅高空雲被觀察到喺下面唔透明嘅雲層上面投射咗陰影。仲有啲高空雲帶以一樣嘅緯度環繞行星。呢啲帶闊 50-150 公里,喺雲層上面大約 50-110 公里[54]。呢啲全部喺對流層,因為冇天氣喺平流層或熱層入面出現。2023年8月,海王星嘅雲層可能因為太陽耀斑消失咗[52]。 哈勃太空望遠鏡同地面望遠鏡三十年嘅觀測表明,海王星嘅雲活動同太陽週期有關,而唔係同行星自己嘅季節有關[55][56]。
海王星嘅光譜表明,由於甲烷畀紫外線光解嘅產物嘅凝結,佢嘅平流層下部分模糊咗[51][40]。平流層亦都有微量一氧化碳同氰化氫[51][57]。由於烴濃度升高,海王星嘅平流層暖過天王星嘅平流層[51]。
由於未知原因,海王星嘅熱層有 750K 嘅異常高溫[58][59]。海王星離太陽太遠,紫外線輻射產生唔到熱。佢咁熱嘅原因可能係大氣同行星磁場入面嘅離子產生相互作用。亦有可能係來自內部並喺大氣入面消散嘅重力波。熱層有微量二氧化碳和水,可能由隕石同塵埃等行星外嘅來源沉積嘅[53][57]。
磁層
[編輯]海王星同天王星嘅磁層好似,磁場同自轉軸差47°,偏離核心至少0.55半徑,離行星中心點約13,500公里。磁場可能由導電液體對流流體運動產生[53],並產生發電機作用[60]。
海王星嘅弓形激波(磁層減緩太陽風嘅地方)喺行星半徑34.9倍嘅距離,磁層頂壓力同太陽風喺行星半徑23-26.5倍距離,而磁層最尾嗰度至少延伸到行星半徑72倍嘅距離,甚至去到更遠[62]。
氣候
[編輯]海王星天氣特點係極端嘅風暴,風速達到近600米/秒(2200公里/小時),幾乎達到超音速[63]。更典型嘅係,透過跟蹤持續雲嘅運動,風速已經顯示出由東向20米/秒到西向325米/秒不等[64]。海王星上嘅大部分風都朝着與行星自轉相反嘅方向移動。
海王星同天王星嘅不同之處就喺佢典型氣象活動水平。航行者2號喺1989年飛越海王星嗰陣觀察倒天氣現象[65],但喺1986年飛越天王星嗰陣冇。
2007年,啲人發現海王星南極比表面平均溫度高大約10°C,溫差足以令海王星嘅甲烷逃逸到南極附近嘅天空[66],而其他區域嘅甲烷係被凍住咗嘅。噉係因為海王星嘅軌道傾角令南極喺40年入面受到太陽光照住。隨住海王星移動,南極會逐漸變暗,北極會變光,令甲烷走去北極度[67][68]。
風暴
[編輯]1989年,NASA嘅航行者2號發現咗大黑斑,佢係一個橫跨 13,000 公里 × 6,600 公里[65]嘅反氣旋風暴系統,並同木星嘅大紅斑相似。1994年11月2號,哈勃太空望遠鏡睇唔到大黑斑,反而喺海王星嘅北半球發現咗類似大黑斑嘅新風暴[69]。
另一場叫 "Scooter" 嘅風暴,係喺比大黑斑更南邊嘅白色雲團。呢個暱稱喺1989年航行者2號探測海王星之前嗰幾個月首次出現,當時觀察到佢嘅移動速度仲快過大黑斑[70]。小暗斑係個南方氣旋風暴,亦都係1989年探測期間觀察到第二勁嘅風暴。當初佢睇落全黑,但當航行者2號接近行星嗰陣,佢出現咗個明亮核心,並且可以喺大多數最高解析度圖像入面見到[71]。2018年,一個新啲嘅主黑斑同細啲嘅黑斑被識別同研究[72]。2023年,人類首次喺地球表面對海王星黑斑觀測[73]。
海王星嘅黑斑被認為係喺對流層入面出現,海拔低過光啲嘅雲層特徵[74],所以佢哋喺上層雲層入面以孔洞嘅形式出現。由於佢哋可以持續幾個月,因此佢哋被認為係渦旋結構[54]。喺對流層頂層周圍形成嘅更加光同持久嘅甲烷雲通常同海王星嘅黑點相關[75]。伴雲嘅持續存在表明,一啲之前出現過嘅暗點可能會繼續以氣旋嘅形式存在,但就唔再係可見嘅暗特徵。當黑斑遷移得太近赤道或可能透過其他未知機制嗰陣,它們可能會消失[76]。
內熱
[編輯]海王星嘅天氣變化比天王星更加多樣化,部分原因係因為海王星嘅內熱更高。海王星對流層上方嘅溫度低至 51.8K (-221.3ºC)。喺大氣壓力1bar嘅深度,溫度有72K (-201.15ºC)[77]。喺氣體層更深嘅地方,溫度穩定噉上升,但同天王星一樣,熱量嘅來源未知,但有更大嘅差異:天王星幅射嘅能量係佢喺太陽度接收嘅能量嘅1.1倍[78],但海王星有2.61倍[79]。海王星比天王星遠50%以上,仲只係接收到40%嘅陽光[51],但佢嘅內能就可以驅動太陽系最快嘅行星風。根據海王星內部嘅熱特性,海王星形成留低嘅熱量可能足以解釋佢而家嘅熱流,但噉就難以解釋天王星缺乏內部熱量而又保持兩粒行星之間嘅相似嘅原因[80]。
衛星
[編輯]海王星已知有16粒衛星[2][81]。海衛一係最大嘅海王星衛星,亦係唯一一粒質量夠大做到球體嘅海王星衛星,佢喺海王星被人發現17日之後被人發現。海衛一有個逆行軌道,係被海王星捕獲而唔係原地形成嘅。佢可能係柯伊伯帶嘅一粒矮行星[82]。由於佢離海王星夠近,所以佢同海王星潮汐鎖定,由於潮汐加速,佢緩慢噉向內盤旋,最後喺大約36億年後達到洛希極限[83]。海衛一係到而家為止喺太陽系入面測量倒嘅最涷天體[84],估計溫度係38K(-235 °C)[85]。
1989年7-9月,航行者2號發現咗六粒海王星衛星[86]。其中,形狀唔規則嘅海衞八出名喺佢同佢密度相近嘅天體唔同,佢未被自己嘅引力將佢拉成球形[87]。佢雖然係海王星質量第二大嘅衛星,但都只係得海衛一質量嘅0.25%。海衞三、海衞四、海衞五同海衞六軌道喺海王星環入面,海衞七喺1981年佢擋住恆星嘅時候被人觀察倒,最初以為係行星環嘅弧,但喺1989年航行者2號再觀察先發現係衛星。
2004年公佈咗2002-2003年發現咗嘅五粒新衛星[88][89]。2013年,通過組合多張哈勃圖像,發現咗一粒新衛星同海王星最細嘅衛星海衞十四[90]。
因為海王星個名係羅馬海神,佢嘅衛星以較低級海神命名[30]。
環
[編輯]海王星有一個行星環系統,儘管比土星嗰個冇咁重要。環可能由涂有矽酸鹽或碳基材料嘅冰粒組成,好可能令佢哋具有微紅嘅色調[91]。三個主要環係距離海王星中心63,000公里嘅窄亞當斯環,53,000公里嘅Le Verrier環同42,000公里嘅更闊,更暗嘅加勒環。Le Verrier Ring嘅一個微弱嘅向外延伸被命名為Lassell,佢嘅外緣以57,000公里嘅Arago環為界[92]。
呢啲行星環中嘅第一個係喺1968年由Edward Guinan領導嘅一個團隊發現嘅[93][94]。
最外層嘅環亞當斯(Adams)包含五條突出嘅弧,而家被命名為 Courage、Liberté、Egalité1、Egalité2同Fraternité(勇氣,自由,平等同埋博愛)[95]。
探測
[編輯]航行者2號係唯一一架訪問過海王星嘅航天器。佢喺1989年8月25號最近海王星[96][97][98]。佢以大約40,000公里嘅距離飛越海衛一[99]。從航行者2號傳返地球嘅圖像成為1989年PBS通宵節目Neptune All Night嘅基礎[100]。
航天器驗證咗行星周圍磁場嘅存在,並發現磁場偏離中心並以類似天王星周圍磁場嘅方式傾斜。海王星嘅自轉周期係使用無線電輻射嘅測量嚟確認嘅,航行者2號仲影到海王星有一個活躍天氣系統並發現咗六粒新衛星同海王星環[101],粒行星被證明有唔止一個環[102]。
今次飛越仲提供埋海王星質量嘅第一次精確測量,發現比以前計算嘅少0.5%。呢個新數字反駁咗一個假設,即一個未被發現嘅行星X影響海王星同天王星嘅軌道[103][104]。
參考
[編輯]- ↑ "Neptune". Solarviews. 喺2007年8月13號搵到.
- ↑ 2.00 2.01 2.02 2.03 2.04 2.05 2.06 2.07 2.08 2.09 2.10 2.11 2.12 2.13 2.14 2.15 2.16 Williams, Dr. David R. (2004年9月1號). "Neptune Fact Sheet". NASA. 喺2007年8月14號搵到.
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- ↑ 軌道參數指嘅係海王星系統嘅重心,同埋係精確J2000曆元入面嘅瞬時密切值。重心量已知係因為對比嘅係行星中心,佢哋無受到嚟自衛星運動影響導致每日唔同嘅可觀變化。
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The clear positive correlation we find between cloud activity and Solar Lyman-Alpha (121.56 nm) irradiance lends support to the theory that the periodicity in Neptune’s cloud activity results from photochemical cloud/haze production triggered by Solar ultraviolet emissions.
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: Check|s2cid=
value (help) - ↑ 57.0 57.1 引用錯誤 無效嘅
<ref>
標籤;無文字提供畀叫做Encrenaz 2003
嘅參照 - ↑ Broadfoot, A.L.; Atreya, S.K.; Bertaux, J.L.; 等 (1999). "Ultraviolet Spectrometer Observations of Neptune and Triton" (PDF). Science. 246 (4936): 1459–66. Bibcode:1989Sci...246.1459B. doi:10.1126/science.246.4936.1459. PMID 17756000. S2CID 21809358. 原先內容歸檔 (PDF)喺28 May 2008. 喺12 March 2008搵到.
- ↑ 引用錯誤 無效嘅
<ref>
標籤;無文字提供畀叫做Herbert & Sandel 1999
嘅參照 - ↑ Stanley, Sabine; Bloxham, Jeremy (11 March 2004). "Convective-region geometry as the cause of Uranus' and Neptune's unusual magnetic fields". Nature. 428 (6979): 151–53. Bibcode:2004Natur.428..151S. doi:10.1038/nature02376. PMID 15014493. S2CID 33352017.
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- ↑ Cruikshank, Dale P. (1996). Neptune and Triton. University of Arizona Press. 703–804. ISBN 978-0-8165-1525-7.
- ↑ Blue, Jennifer (8 December 2004). "Nomenclature Ring and Ring Gap Nomenclature". Gazetteer of Planetary Nomenclature. USGS
- ↑ Wilford, John N. (10 June 1982). "Data Shows 2 Rings Circling Neptune". 紐約時報.
- ↑ Guinan, E.F.; Harris, C.C.; Maloney, F.P. (1982). "Evidence for a Ring System of Neptune". Bulletin of the American Astronomical Society. 14: 658. Bibcode:1982BAAS...14..658G.
- ↑ Cox, Arthur N. (2001). Allen's Astrophysical Quantities. Springer. ISBN 978-0-387-98746-0.
- ↑ "Voyager Steered Toward Neptune". Ukiah Daily Journal. March 15, 1987. 喺December 6, 2017搵到.
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- ↑ Nardo 2002, p. 15
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- ↑ Phillips, Cynthia (5 August 2003). "Fascination with Distant Worlds". SETI Institute.
- ↑ National Aeronautics and Space Administration "Neptune Moons" 互聯網檔案館嘅歸檔,歸檔日期2020年4月10號,. NASA Science: Solar System Exploration. Updated December 6, 2017. Accessed December 12, 2018.
- ↑ Stone, E.C.; Miner, E.D. (1989). "The Voyager 2 Encounter with the Neptunian System". Science. 246 (4936): 1417–21. Bibcode:1989Sci...246.1417S. doi:10.1126/science.246.4936.1417. PMID 17755996. S2CID 9367553.
- ↑ Tom Standage (2000). The Neptune File: A Story of Astronomical Rivalry and the Pioneers of Planet Hunting. New York: Walker. p. 188. ISBN 978-0-8027-1363-6.
- ↑ Chris Gebhardt; Jeff Goldader (20 August 2011). "Thirty-four years after launch, Voyager 2 continues to explore". NASA Spaceflight.