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太陽系外惑星の発見方法 Metody poszukiwania planet pozasłonecznych Méthodes de détection des exoplanètes 외계 행성 탐사방법 Upptäcktsmetoder för exoplaneter 系外行星偵測法 Metodi di individuazione di pianeti extrasolari Metode pendeteksian eksoplanet Métodos de detecção de exoplanetas طرق اكتشاف الكواكب خارج المجموعة الشمسية Métodos de detección de planetas extrasolares Methoden om exoplaneten te vinden Methods of detecting exoplanets Методы обнаружения экзопланет
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任何行星相對於其母恆星都是極其微弱的光源。要在母恆星耀眼的光輝內同時檢測出這種微弱的光源,都有其內在的困難。因為這種緣故,只有很少的太陽系外行星被直接觀測到。 取而代之的,天文學家通常都使用間接的方法來偵測太陽系外的行星。目前,有好幾種間接的方法都成功地偵測到了行星。 En planet i omloppsbana runt en annan stjärna, en så kallad extrasolär planet eller exoplanet, kan vara mycket svår att visuellt identifiera i skenet från sin sol (eller sina solar). Även om planeten som sådan har ett mycket högt albedovärde, kommer detta relativt svaga ljus att försvinna i det utstrålade ljuset från den sol eller de solar planeten kretsar runt. För att kunna finna fler och mindre exoplaneter har astronomer tvingats ta fram nya och bättre metoder för att indirekt detektera dessa. Any planet is an extremely faint light source compared to its parent star. For example, a star like the Sun is about a billion times as bright as the reflected light from any of the planets orbiting it. In addition to the intrinsic difficulty of detecting such a faint light source, the light from the parent star causes a glare that washes it out. For those reasons, very few of the exoplanets reported as of April 2014 have been observed directly, with even fewer being resolved from their host star. Een planeet zal vergeleken met de ster uit haar stelsel altijd een extreem zwakke lichtbron zijn. Een ster als de zon is bijvoorbeeld een miljard keer zo fel als elk van de planeten die om haar heen draaien. Behalve dat het altijd lastig is om zo'n zwakke lichtbron waar te kunnen nemen, zal de felle schittering van zo'n begeleidende ster de planeet ook verbloemen. Om deze redenen zijn slechts heel weinig van de bewezen exoplaneten direct geobserveerd en nog minder zijn afzonderlijk van een ster waargenomen. In plaats daarvan gebruiken astronomen gewoonlijk indirecte methoden om planeten te ontdekken. Op 28 januari 2021 waren er 4341 exoplaneten door NASA vastgesteld. En astronomie, la recherche des exoplanètes fait appel à plusieurs méthodes de détection. La majorité de ces méthodes sont à l'heure actuelle indirectes, puisque la proximité de ces planètes avec leur étoile est si grande que leur lumière est complètement noyée dans celle de l'étoile. طرق اكتشاف الكواكب خارج المجموعة الشمسية هي أساليب غير مباشرة يلجاء إليها علماء الفلك للكشف عن الكواكب خارج المجموعة الشمسية نظرا لكون الضوء المنبعث من الكوكب خافتا مقارنة بالضوء الصادر عن النجم مما يجعل اكتشاف الكوكب صعباً، خاصةً وأن الضوء المنبعث من النجم يغلب على الضوء المستقبل من الكوكب. ولهذا فقد انحصر عدد الكواكب المكتشفة خارج المجموعة الشمسية والتي رؤيت مباشرة في عدد قليل حتى الآن. اعتبارا من عام 2016، حققت عدة طرق مختلفة غير مباشرة النجاح في هذا المجال. 외계 행성 탐사방법은 외계행성을 발견하는 방법과 예시를 담은 문서이다. 대부분 직접적인 증거보다 간접적인 증거를 찾아 외계행성을 추론하는 경우다. Планеты, обращающиеся около других звёзд, являются источниками очень слабого света в сравнении с родительской звездой, поэтому прямое наблюдение и обнаружение экзопланет является довольно сложной задачей. Помимо значительной сложности обнаружения такого слабого источника света, возникает дополнительная проблема, связанная с тем, что яркость родительской звезды на много порядков превышает звёздную величину планеты, светящуюся отражённым от родительской звезды светом, и тем самым делает оптические наблюдения экзопланет сверхсложными для наблюдений. Из-за этого только около 5% от всех экзопланет, обнаруженных к ноябрю 2011 года, наблюдались прямым методом. Все остальные планеты найдены косвенными методами, заключающимися в обнаружении влияния планеты на окружающие тела. 本項では太陽系外惑星の発見方法について述べる。惑星は自ら光る恒星と比べて、非常にかすかな光を反射しているに過ぎないため外部から見ると非常に発見しにくい天体である。例えば、太陽のような恒星は、惑星が反射する光の約10億倍の明るさを持つ。そのようなわずかな光を検出するという本質的な難しさに加え、恒星の光が惑星からの光をかき消してしまう場合もある。こうした理由から、2014年4月までに発見された太陽系外惑星のほとんどは直接観測されていない。 太陽系外惑星の発見方法には惑星を直接観測することで発見する直接法(英語: Direct method)と、惑星が恒星に及ぼす影響などから間接的に惑星を発見する間接法(英語: Indirect method)とに分けられる。現在の観測技術で太陽系外惑星を直接観測することは困難であり、2020年時点で存在が知られている太陽系外惑星の大部分は間接法によって発見されている。 I metodi di individuazione di pianeti extrasolari sono diversi e si sono evoluti nel corso degli anni, permettendo oggi di scoprire nuovi pianeti a un ritmo sempre crescente. Le metodologie si possono dividere in due classi principali: * rilevamento diretto; * rilevamento indiretto. Planety pozasłoneczne są bardzo trudne do bezpośredniego zaobserwowania, ponieważ zwykle ich blask ginie w świetle gwiazdy macierzystej. Dlatego do wykrywania takich planet korzysta się z pośrednich metod. Poniżej przedstawiono metody, które do tej pory okazały się skuteczne, oraz niektóre metody będące w fazie projektów. Cualquier planeta constituye una fuente de luz extremadamente tenue en comparación con la estrella alrededor de la que órbita (estrella madre). Detectar una fuente de luz tan tenue es sumamente difícil y el resplandor de la luz de la estrella madre lo hace aún más complicado. Por estos motivos, menos del 5% de los planetas extrasolares conocidos en febrero de 2014 se han detectado mediante observación directa.​ Qualquer planeta é uma fonte de luz extremamente fraca em comparação com sua estrela hospedeira. Por exemplo, uma estrela como o Sol é cerca de um bilhão de vezes mais brilhante que a luz refletida de qualquer um dos planetas que a orbitam. Além da dificuldade intrínseca de detectar uma fonte de luz tão fraca, a luz da estrela hospedeira causa um brilho que a apaga. Por essas razões, muito poucos dos exoplanetas relatados em abril de 2014 foram observados diretamente, com ainda menos sendo resolvidos de sua estrela hospedeira. Planet menjadi sumber cahaya yang sangat redup bila dibandingkan dengan bintang induknya. Misalnya, bintang seperti Matahari memiliki kecerahan sekitar satu miliar kali lebih terang daripada cahaya yang dipantulkan dari planet mana pun yang mengorbitnya. Selain kesulitan intrinsik untuk mendeteksi sumber cahaya yang redup tersebut, cahaya dari bintang induk menyilaukan daerah di sekitarnya dan menutupi cahaya dari planet-planet. Karena alasan tersebut, sangat sedikit eksoplanet yang dilaporkan telah diamati secara langsung, bahkan lebih sedikit lagi yang telah diamati terlepas dari bintang induknya.
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Planet menjadi sumber cahaya yang sangat redup bila dibandingkan dengan bintang induknya. Misalnya, bintang seperti Matahari memiliki kecerahan sekitar satu miliar kali lebih terang daripada cahaya yang dipantulkan dari planet mana pun yang mengorbitnya. Selain kesulitan intrinsik untuk mendeteksi sumber cahaya yang redup tersebut, cahaya dari bintang induk menyilaukan daerah di sekitarnya dan menutupi cahaya dari planet-planet. Karena alasan tersebut, sangat sedikit eksoplanet yang dilaporkan telah diamati secara langsung, bahkan lebih sedikit lagi yang telah diamati terlepas dari bintang induknya. Oleh karena itu, para astronom umumnya harus menggunakan metode tidak langsung untuk mendeteksi planet-planet ekstrasurya. Pada tahun 2016, beberapa metode tidak langsung yang berbeda telah membuahkan hasil dalam mendeteksi planet-planet tersebut. Een planeet zal vergeleken met de ster uit haar stelsel altijd een extreem zwakke lichtbron zijn. Een ster als de zon is bijvoorbeeld een miljard keer zo fel als elk van de planeten die om haar heen draaien. Behalve dat het altijd lastig is om zo'n zwakke lichtbron waar te kunnen nemen, zal de felle schittering van zo'n begeleidende ster de planeet ook verbloemen. Om deze redenen zijn slechts heel weinig van de bewezen exoplaneten direct geobserveerd en nog minder zijn afzonderlijk van een ster waargenomen. In plaats daarvan gebruiken astronomen gewoonlijk indirecte methoden om planeten te ontdekken. Op 28 januari 2021 waren er 4341 exoplaneten door NASA vastgesteld. Qualquer planeta é uma fonte de luz extremamente fraca em comparação com sua estrela hospedeira. Por exemplo, uma estrela como o Sol é cerca de um bilhão de vezes mais brilhante que a luz refletida de qualquer um dos planetas que a orbitam. Além da dificuldade intrínseca de detectar uma fonte de luz tão fraca, a luz da estrela hospedeira causa um brilho que a apaga. Por essas razões, muito poucos dos exoplanetas relatados em abril de 2014 foram observados diretamente, com ainda menos sendo resolvidos de sua estrela hospedeira. Em vez disso, os astrônomos geralmente tiveram que recorrer a métodos indiretos para detectar exoplanetas. A partir de 2016, vários métodos indiretos diferentes renderam sucesso. Any planet is an extremely faint light source compared to its parent star. For example, a star like the Sun is about a billion times as bright as the reflected light from any of the planets orbiting it. In addition to the intrinsic difficulty of detecting such a faint light source, the light from the parent star causes a glare that washes it out. For those reasons, very few of the exoplanets reported as of April 2014 have been observed directly, with even fewer being resolved from their host star. Instead, astronomers have generally had to resort to indirect methods to detect extrasolar planets. As of 2016, several different indirect methods have yielded success. 本項では太陽系外惑星の発見方法について述べる。惑星は自ら光る恒星と比べて、非常にかすかな光を反射しているに過ぎないため外部から見ると非常に発見しにくい天体である。例えば、太陽のような恒星は、惑星が反射する光の約10億倍の明るさを持つ。そのようなわずかな光を検出するという本質的な難しさに加え、恒星の光が惑星からの光をかき消してしまう場合もある。こうした理由から、2014年4月までに発見された太陽系外惑星のほとんどは直接観測されていない。 太陽系外惑星の発見方法には惑星を直接観測することで発見する直接法(英語: Direct method)と、惑星が恒星に及ぼす影響などから間接的に惑星を発見する間接法(英語: Indirect method)とに分けられる。現在の観測技術で太陽系外惑星を直接観測することは困難であり、2020年時点で存在が知られている太陽系外惑星の大部分は間接法によって発見されている。 Planety pozasłoneczne są bardzo trudne do bezpośredniego zaobserwowania, ponieważ zwykle ich blask ginie w świetle gwiazdy macierzystej. Dlatego do wykrywania takich planet korzysta się z pośrednich metod. Poniżej przedstawiono metody, które do tej pory okazały się skuteczne, oraz niektóre metody będące w fazie projektów. 외계 행성 탐사방법은 외계행성을 발견하는 방법과 예시를 담은 문서이다. 대부분 직접적인 증거보다 간접적인 증거를 찾아 외계행성을 추론하는 경우다. Cualquier planeta constituye una fuente de luz extremadamente tenue en comparación con la estrella alrededor de la que órbita (estrella madre). Detectar una fuente de luz tan tenue es sumamente difícil y el resplandor de la luz de la estrella madre lo hace aún más complicado. Por estos motivos, menos del 5% de los planetas extrasolares conocidos en febrero de 2014 se han detectado mediante observación directa.​ Por ello, los astrónomos han tenido que recurrir por lo general a métodos indirectos para detectar los planetas extrasolares. Hasta la fecha, los siguientes métodos indirectos se han demostrado útiles. 任何行星相對於其母恆星都是極其微弱的光源。要在母恆星耀眼的光輝內同時檢測出這種微弱的光源,都有其內在的困難。因為這種緣故,只有很少的太陽系外行星被直接觀測到。 取而代之的,天文學家通常都使用間接的方法來偵測太陽系外的行星。目前,有好幾種間接的方法都成功地偵測到了行星。 En planet i omloppsbana runt en annan stjärna, en så kallad extrasolär planet eller exoplanet, kan vara mycket svår att visuellt identifiera i skenet från sin sol (eller sina solar). Även om planeten som sådan har ett mycket högt albedovärde, kommer detta relativt svaga ljus att försvinna i det utstrålade ljuset från den sol eller de solar planeten kretsar runt. För att kunna finna fler och mindre exoplaneter har astronomer tvingats ta fram nya och bättre metoder för att indirekt detektera dessa. طرق اكتشاف الكواكب خارج المجموعة الشمسية هي أساليب غير مباشرة يلجاء إليها علماء الفلك للكشف عن الكواكب خارج المجموعة الشمسية نظرا لكون الضوء المنبعث من الكوكب خافتا مقارنة بالضوء الصادر عن النجم مما يجعل اكتشاف الكوكب صعباً، خاصةً وأن الضوء المنبعث من النجم يغلب على الضوء المستقبل من الكوكب. ولهذا فقد انحصر عدد الكواكب المكتشفة خارج المجموعة الشمسية والتي رؤيت مباشرة في عدد قليل حتى الآن. اعتبارا من عام 2016، حققت عدة طرق مختلفة غير مباشرة النجاح في هذا المجال. I metodi di individuazione di pianeti extrasolari sono diversi e si sono evoluti nel corso degli anni, permettendo oggi di scoprire nuovi pianeti a un ritmo sempre crescente. Le metodologie si possono dividere in due classi principali: * rilevamento diretto; * rilevamento indiretto. Nella classe del rilevamento diretto si includono tutte le tecniche che permettono di osservare direttamente al telescopio questi pianeti. Nella classe del rilevamento indiretto ricadono quelle tecniche che permettono di individuare un pianeta a partire dagli effetti che esso induce (o vengono indotti) sulla (o dalla) stella ospite. Per confermare un pianeta e meglio definirne le caratteristiche fisiche è necessario l'utilizzo di più tecniche differenti. Al momento attuale il metodo di ricerca più fruttuoso è quello delle velocità radiali che ha fornito 203 pianeti sui circa 500 noti, seguito da quello dei transiti. Già nel 1955 Otto Struve aveva prospettato la possibilità di scoprire sistemi planetari extrasolari proprio con questi due metodi. Tutti i pianeti extrasolari scoperti al 31 agosto 2004 (ascisse semiasse maggiore, ordinate masse gioviane):I puntini blu rappresentano pianeti scoperti con il Metodo delle Velocità radiali.In rosso quelli con metodo del transito.in giallo con la microlente gravitazionale.L'immagine mostra anche i limiti delle capacità di rilevamento dei prossimi strumenti (linee colorate), sia terrestri che spaziali, dal 2006 al 2015.Infine l'immagine mostra anche la posizione dei pianeti del sistema solare sono i pallini più grandi con l'iniziale del nome inglese. Планеты, обращающиеся около других звёзд, являются источниками очень слабого света в сравнении с родительской звездой, поэтому прямое наблюдение и обнаружение экзопланет является довольно сложной задачей. Помимо значительной сложности обнаружения такого слабого источника света, возникает дополнительная проблема, связанная с тем, что яркость родительской звезды на много порядков превышает звёздную величину планеты, светящуюся отражённым от родительской звезды светом, и тем самым делает оптические наблюдения экзопланет сверхсложными для наблюдений. Из-за этого только около 5% от всех экзопланет, обнаруженных к ноябрю 2011 года, наблюдались прямым методом. Все остальные планеты найдены косвенными методами, заключающимися в обнаружении влияния планеты на окружающие тела. En astronomie, la recherche des exoplanètes fait appel à plusieurs méthodes de détection. La majorité de ces méthodes sont à l'heure actuelle indirectes, puisque la proximité de ces planètes avec leur étoile est si grande que leur lumière est complètement noyée dans celle de l'étoile.
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