سیارکها (به انگلیسی: Asteroid) اجسام کوچکی هستند که از سنگ یا فلز ساخته شدهاند. سیارکها معمولاً اجسام نامنظمی هستند و بر گرد خورشید حرکت میکنند. میلیونها سیارک در منظومه خورشیدی ما وجود دارند. بسیاری از آنها میان مدار بهرام (مریخ) و مدار هرمز (مشتری) قرار گرفتهاند و گرد خورشید میگردند. دستهای دیگر از آنها در مکانهای دیگر منظومه خورشیدی یافت میشوند. به نظر میرسد علت اینکه اغلب آنها در فاصلهٔ مریخ و مشتری دیده میشوند این است که احتمالاً در مدار بین این دو سیاره، سیارهٔ دیگری نیز وجود داشتهاست که به علت گرانش شدید مشتری متلاشی شدهاست و سیارکها پدید آمده باشند.
به سیارکهایی که بر اثر نیروی گرانش سیارهها در مداری گیر افتاده باشند «سیارک اسیر» میگویند. در این صورت سیارهٔ نامبرده به گرد سیاره بزرگتر میگردد.
فقط یک سیارک به نام «۴ وستا»، که دارای سطح نسبتاً بازتابی است، معمولاً با چشم غیر مسلح قابل مشاهده است، و این تنها در آسمانهای بسیار تاریک در هنگام قرار گرفتن در موقعیت مناسب امکانپذیر است. به ندرت، سیارکهای کوچک که از نزدیکی زمین عبور میکنند، آن هم برای برای مدت کوتاهی، ممکن است با چشم غیر مسلح قابل مشاهده باشند.از فوریه ۲۰۲۰، مرکز Minor Planet دادههای مربوط به تقریباً ۸۵۸۰۰۰ شیء در منظومه شمسی داخلی و خارجی را در اختیار داشت، از این تعداد حدود ۵۴۲٬۰۰۰ مورد اطلاعات کافی برای تعیین شمارههای اختصاصی داشتند.
در آغازین روزهای ژانویهٔ ۱۸۰۱ جوزپه پیاتسی (۷ ژوئیهٔ ۱۷۴۶–۲۲ ژوئیهٔ ۱۸۲۶) جرمی را در آسمان رصد نمود که ابتدا یک شهاب سنگ به نظر میرسید ولی زمانی که مدار آن بهدرستی تعیین گردید، مشخص شد که سیاره بسیار کوچکی است، آنقدر کوچک که آن را در رده جدیدی به نام سیارکها دستهبندی کردند. پیاتسی آن را سرس نامید. تا چند سال بعد سه سیارک جدید دیگر کشف شدند و تا پایان آن قرن صدها عدد از آنها شناسایی شده بودند. تا به امروز تعداد این سیارکها به چند صد هزار رسیدهاست و هنوز اکتشاف آنها ادامه دارد. تعدادی از سیارکها چنان کوچکند که از زمین قابل رؤیت نیستند اما بزرگترین آنها همان سِرِس است که شماره یک را بر پیشانی خود دارد.
همینکه مدار سیارکی مشخص میگردد، عددی به ترتیبِ زمانِ کشف بدان نسبت داده میشود و به دنبال آن نامی میآورند که نام را معمولاً کاشف برمیگزیند؛ مثلاً ۱ سِرِس. در آغاز نامهای زنانه از اسطورههای یونان و روم انتخاب میشد. بعدها نامهایی از نمایشنامههای شکسپیر و اپراهای واگنر برگزیده شدند. بسیاری از سیارکها را کاشفان به نامهای زنان، دوستان و حتی سگها و گربههای خود نامیدند. همواره نامهایی مؤنث بهکار رفتهاست، جز در مورد چند سیارک که مدارهایی نامتعارف دارند، نامهای مذکر نهاده شدهاست.
کمربند سیارکها همانطور که گفته شد ناحیهای بین مریخ و مشتری است که سیارکها در آن قرار دارند و بیشتر به مریخ نزدیک است تا به مشتری و سیارکهای این ناحیه در حدود ۳۰۰ – ۶۰۰ میلیون ک م با خورشید فاصله دارند. (ناحیه داخلی منظومه شمسی سیارکها). مدار سیارکها بیضی شکل هست. بعضی از آنها هنگام گردش از داخل ناهید عبور میکنند و بعضی در دام گرانش مشتری گیر کرده و از کمربند سیارکها خارج میشوند و بعضی در دام مریخ میافتند یا با یکدیگر برخورد میکنند. قمرهای فوبوس و دیموس مریخ ممکن است سیارکهایی باشند که در دام آن افتادهاند.
همانطور که در شکل میبینید این کمربند شامل سه بخش دیگر نیز میباشد:
Trojans: تروجانها یا سیارکهای تراوایی مدار مشترک با مشتری دارند و با هر یک دور مشتری یک دور میزنند
Hildas: هر دو دور مشتری به دور خورشید برابر ۳ دور آنها به دور خورشید است.
Greeks: تعداد دور این سیارکها متغیر است.
علاوهبر اینها سه مدار دیگر نیز وجود دارد که برخی سیارکها در آن قرار دارند که در شکل زیر مشخص است:
آپولوها: مدار زمین را قطع میکنند
آتنها: همیشه از زمین به خورشید نزدیکترند
آمورها: سیارکهای بین زمین و مریخ
تا عصر مسافرت در فضا، اشیاء موجود در کمربند سیارکی حتی در بزرگترین تلسکوپها نورهای مبهمی بودند و شکل و جنس آنها به صورت رمز و راز باقی مانده بود. بهترین تلسکوپهای مدرن نصب شده روی زمین و تلسکوپ فضایی هابل میتوانند مقدار کمی از جزئیات را بر روی سطح بزرگترین سیارکها نشان دهند، اما حتی این موارد نیز نمایی کمی بهتر از حبابهای فازی نشان میدهند. اطلاعات محدودی در مورد شکل و ترکیبات سیارکها را میتوان از منحنیهای نوری آنها (تغییر در میزان روشنایی در چرخش آنها) و از خصوصیات طیفی آنها استنباط کرد و اندازه سیارکها را میتوان با زمانبندی طول انقباضات ستاره (هنگامی که یک سیارک مستقیماً از جلوی یک ستاره عبور میکند) تخمین زد. تصویربرداری راداری میتواند اطلاعات خوبی در مورد اشکال سیارکها و پارامترهای مداری و چرخشی به خصوص در مورد سیارکهای نزدیک به زمین بدست آورد. از نظر delta-v و الزامات پیشرانه، NEOها راحتتر از ماه قابل دسترسی هستند.
سیارکها معمولاً بر اساس دو معیار طبقهبندی میشوند: ویژگیهای مدار آنها و ویژگیهای طیف بازتاب آنها.
بسیاری از سیارکها بر اساس ویژگیهای مداری آنها در گروهها و خانوادهها قرار داده شدهاند. جدا از گستردهترین تقسیمات، مرسوم است که نام گروه سیارکها را با توجه به نام اولین عضو آن گروه که کشف شده نام گذاری کنند. گروهها عموماً ا پیوندهای قابل گسست تری نسبت به خانواده سیارکها، که ناشی از انفجار یک سیارک بزرگ والد در گذشته هستند، دارند. شناسایی خانوادهها در کمربند اصلی سیارک معمول تر و آسانتر است، اما چندین خانواده کوچک در میان تروجانهای مشتری گزارش شدهاست. خانوادههای کمربند اصلی برای اولین بار در سال ۱۹۱۸ توسط کیوتوگوگو هیرایاما شناخته شدند و اغلب به احترام وی خانواده هیرایاما خوانده میشوند.
در سال ۱۹۷۵، یک سیستم طبقهبندی سیارک مبتنی بر رنگ، سپیدایی و خط طیف نوری توسط کلارک چاپمن، دیوید موریسون و بن زلنر توسعه یافت. تصور میشود این خصوصیات با ترکیب مواد سطح سیارک مطابقت داشته باشد. سیستم طبقهبندی اصلی دارای سه دسته است: انواع C برای اشیاء کربنی تیره (شامل ۷۵٪ سیارکهای شناخته شده)، نوع S برای اشیاء سنگی (شامل ۱۷٪ سیارکهای شناخته شده) و U برای آنهایی که در هیچیک از دو گروه قبلی جای نمیگرفتند. از آنجا که این طبقهبندی شامل بسیاری از انواع سیارکها است، این طبقهبندی همواره گسترش یافتهاست. با مطالعه بیشتر سیارکها، تعداد آنها همچنان رو به رشد است.
تا سال ۱۹۹۰ تنها ۳ راه برای اندازهگیری قطر سیارکها وجود داشت.
روش اول :استفاده از تلسکوپ و اندازهگیری فاصله آن از خورشید و محاسبه مقدار نوری که از خورشید بر سطح سیارک تابیده شده یا مقدار انرژی گرمایی آزاد شده از آن (میزان نور منعکس شده یا گرمای آزاد شده از سیارک متناسب با اندازه آن میباشد). روش دوم: استفاده از تلسکوپ و محاسبه مدت زمانی که سیارک از دید خارج شده و به پشت یک ستاره رفته و ایجاد سایه کند.
روش سوم: استفاده از رادیو تلسکوپها و تهیه عکس از سیارک.
از سال ۱۹۹۱ دانشمندان از روش چهارمی نیز استفاده نمودهاند که از دقت بیشتری در مقایسه با روشهای فوق بر خوردار است؛ و آن استفاده از مأموریتها و اکتشافات فضایی میباشد(Space Probes). در آن سال اولین مأموریت فضایی آمریکا برای عکسبرداری از سیارکها آغاز شد و سیارک Gaspra اولین سیارکی بود که توسط فضاپیمای گالیله مورد عکسبرداری واقع شد. مأموریت گالیله سیاره مشتری بود که در راه رسیدن به آن باید از کمربند سیارکها عبور میکرد. در سال ۹۶ ناسا مأموریت NEAR (Near Earth Asteroid Rendezvous) را انجام داد که به ۱۲۱۶ کیلومتری سیارک متیلدا رسید. این مأموریت در عین حال اولین موردی بودکه ناسا موفق شد فضاپیمایی را بر روی یک سیارک فرود آورده و اطلاعات وسیعی دربارهٔ ماهیت و منشأ ان کسب نماید. این فضا پیما در فوریه ۲۰۰۱ در ساعت ۳:۰۱ بر روی سیارک eros فرود آمد. در سالهای بعد این فضاپیما به سیارکهای دیگر رسید.
ازمنابع آلی و معدنی موجود در سیارکها میتوان برای تأمین مواد و آب مورد نیاز جهت ساخت تجهیزات فضایی و مداری استفاده نمود. اینک بسیاری از مراکز پژوهشی مرتبط با فناوری فضایی در حال مطالعه امکان سفر به سیارکها و برداشت از ذخایر طبیعی آنها هستند.
به تازگی و با کشف یخ آب بر سطح سیارک تمیس-۲۴، ایدههایی به منظور برداشت آب از آنها جهت استفاده آب مصرفی فضانوردان و تأمین اکسیژن و هیدروژن به وسیلهٔ الکترولیز نمودن آب برای تنفس یا سوخت فضاپیماهای آینده مطرح شدهاست. اگر مدار سفرهای فضایی آینده را بتوان به گونهای طراحی کرد که هر بار سیارک دارای ذخایر یخ آب در مسیر قرار داشته باشد میتوان به سادگی تأسیسات لازم برای یک ایستگاه سوختگیری فضایی را بر سطح آن سیارک بنا نمود. تأسیساتی تمام اتوماتیک که انرژی تابشی خورشید را توسط صفحات خورشیدی دریافت و به الکتریسیته تبدیل نمایند و سپس با استفاده از این انرژی الکتریکی، یخ آب موجود در خرده سیارک را با یک اجاق مایکروویو ساده ذوب کرده و آب حاصله را با یک دستگاه ساده الکترولیز به هیدروژن و اکسیژن تجزیه نمایند. در انتها هیدروژن و اکسیژن به دست آمده در مخازن جدا از هم ذخیره خواهند شد. این طرح هنوز در مرحله ایده قرار داشته و به مرحله عمل نرسیدهاست.
برای اکتشاف معادن در سیارکها باید بتوان روی آنها فرود آمد و این کاری است مشکل و شاید غیرممکن. به این خاطر دانشمندان در اندیشه راهی برای توقف چرخش سیارکهای پیرامون زمین هستند. برای این کار جیپهایی در نظر گرفته شده که با نیروی موشکی کار میکنند. برای یک سیارک با قطر ۱۰۰ متر که ۴ بار در روز حول محور خود میچرخد، ۲۹ تن سوخت نیاز است تا از چرخش بازداشته شود.
An asteroid is a minor planet of the inner Solar System. Historically, these terms have been applied to any astronomical object orbiting the Sun that did not resolve into a disc in a telescope and was not observed to have characteristics of an active comet such as a tail. As minor planets in the outer Solar System were discovered that were found to have volatile-rich surfaces similar to comets, these came to be distinguished from the objects found in the main asteroid belt. Thus the term "asteroid" now generally refers to the minor planets of the inner Solar System, including those co-orbital with Jupiter. Larger asteroids are often called planetoids.
Millions of asteroids exist: many are shattered remnants of planetesimals, bodies within the young Sun's solar nebula that never grew large enough to become planets. The vast majority of known asteroids orbit within the main asteroid belt located between the orbits of Mars and Jupiter, or are co-orbital with Jupiter (the Jupiter trojans). However, other orbital families exist with significant populations, including the near-Earth objects. Individual asteroids are classified by their characteristic spectra, with the majority falling into three main groups: C-type, M-type, and S-type. These were named after and are generally identified with carbon-rich, metallic, and silicate (stony) compositions, respectively. The sizes of asteroids varies greatly; the largest, Ceres, is almost 1,000 km (600 mi) across and massive enough to qualify as a dwarf planet.
Asteroids are somewhat arbitrarily differentiated from comets and meteoroids. In the case of comets, the difference is one of composition: while asteroids are mainly composed of mineral and rock, comets are primarily composed of dust and ice. Furthermore, asteroids formed closer to the sun, preventing the development of cometary ice. The difference between asteroids and meteoroids is mainly one of size: meteoroids have a diameter of one meter or less, whereas asteroids have a diameter of greater than one meter. Finally, meteoroids can be composed of either cometary or asteroidal materials.
Only one asteroid, 4 Vesta, which has a relatively reflective surface, is normally visible to the naked eye, and this is only in very dark skies when it is favorably positioned. Rarely, small asteroids passing close to Earth may be visible to the naked eye for a short time. As of March 2020[update], the Minor Planet Center had data on 930,000 minor planets in the inner and outer Solar System, of which about 545,000 had enough information to be given numbered designations.
The United Nations declared 30 June as International Asteroid Day to educate the public about asteroids. The date of International Asteroid Day commemorates the anniversary of the Tunguska asteroid impact over Siberia, Russian Federation, on 30 June 1908.
In April 2018, the B612 Foundation reported "It is 100 percent certain we'll be hit [by a devastating asteroid], but we're not 100 percent sure when." Also in 2018, physicist Stephen Hawking, in his final book Brief Answers to the Big Questions, considered an asteroid collision to be the biggest threat to the planet. In June 2018, the US National Science and Technology Council warned that America is unprepared for an asteroid impact event, and has developed and released the "National Near-Earth Object Preparedness Strategy Action Plan" to better prepare. According to expert testimony in the United States Congress in 2013, NASA would require at least five years of preparation before a mission to intercept an asteroid could be launched.
The first asteroid to be discovered, Ceres, was originally considered to be a new planet.[a] This was followed by the discovery of other similar bodies, which, with the equipment of the time, appeared to be points of light, like stars, showing little or no planetary disc, though readily distinguishable from stars due to their apparent motions. This prompted the astronomer Sir William Herschel to propose the term "asteroid",[b] coined in Greek as ἀστεροειδής, or asteroeidēs, meaning 'star-like, star-shaped', and derived from the Ancient Greek ἀστήρ astēr 'star, planet'. In the early second half of the nineteenth century, the terms "asteroid" and "planet" (not always qualified as "minor") were still used interchangeably.[c]
Asteroid discovery methods have dramatically improved over the past two centuries.
In the last years of the 18th century, Baron Franz Xaver von Zach organized a group of 24 astronomers to search the sky for the missing planet predicted at about 2.8 AU from the Sun by the Titius-Bode law, partly because of the discovery, by Sir William Herschel in 1781, of the planet Uranus at the distance predicted by the law. This task required that hand-drawn sky charts be prepared for all stars in the zodiacal band down to an agreed-upon limit of faintness. On subsequent nights, the sky would be charted again and any moving object would, hopefully, be spotted. The expected motion of the missing planet was about 30 seconds of arc per hour, readily discernible by observers.
The first object, Ceres, was not discovered by a member of the group, but rather by accident in 1801 by Giuseppe Piazzi, director of the observatory of Palermo in Sicily. He discovered a new star-like object in Taurus and followed the displacement of this object during several nights. Later that year, Carl Friedrich Gauss used these observations to calculate the orbit of this unknown object, which was found to be between the planets Mars and Jupiter. Piazzi named it after Ceres, the Roman goddess of agriculture.
Three other asteroids (2 Pallas, 3 Juno, and 4 Vesta) were discovered over the next few years, with Vesta found in 1807. After eight more years of fruitless searches, most astronomers assumed that there were no more and abandoned any further searches.
However, Karl Ludwig Hencke persisted, and began searching for more asteroids in 1830. Fifteen years later, he found 5 Astraea, the first new asteroid in 38 years. He also found 6 Hebe less than two years later. After this, other astronomers joined in the search and at least one new asteroid was discovered every year after that (except the wartime year 1945). Notable asteroid hunters of this early era were J.R. Hind, A. de Gasparis, R. Luther, H.M.S. Goldschmidt, J. Chacornac, J. Ferguson, N.R. Pogson, E.W. Tempel, J.C. Watson, C.H.F. Peters, A. Borrelly, J. Palisa, the Henry brothers and A. Charlois.
In 1891, Max Wolf pioneered the use of astrophotography to detect asteroids, which appeared as short streaks on long-exposure photographic plates. This dramatically increased the rate of detection compared with earlier visual methods: Wolf alone discovered 248 asteroids, beginning with 323 Brucia, whereas only slightly more than 300 had been discovered up to that point. It was known that there were many more, but most astronomers did not bother with them, some calling them "vermin of the skies", a phrase variously attributed to E. Suess and E. Weiss. Even a century later, only a few thousand asteroids were identified, numbered and named.
Manual methods of the 1900s and modern reporting
Until 1998, asteroids were discovered by a four-step process. First, a region of the sky was photographed by a wide-field telescope, or astrograph. Pairs of photographs were taken, typically one hour apart. Multiple pairs could be taken over a series of days. Second, the two films or plates of the same region were viewed under a stereoscope. Any body in orbit around the Sun would move slightly between the pair of films. Under the stereoscope, the image of the body would seem to float slightly above the background of stars. Third, once a moving body was identified, its location would be measured precisely using a digitizing microscope. The location would be measured relative to known star locations.
These first three steps do not constitute asteroid discovery: the observer has only found an apparition, which gets a provisional designation, made up of the year of discovery, a letter representing the half-month of discovery, and finally a letter and a number indicating the discovery's sequential number (example: 1998 FJ74).
The last step of discovery is to send the locations and time of observations to the Minor Planet Center, where computer programs determine whether an apparition ties together earlier apparitions into a single orbit. If so, the object receives a catalogue number and the observer of the first apparition with a calculated orbit is declared the discoverer, and granted the honor of naming the object subject to the approval of the International Astronomical Union.
There is increasing interest in identifying asteroids whose orbits cross Earth's, and that could, given enough time, collide with Earth (see Earth-crosser asteroids). The three most important groups of near-Earth asteroids are the Apollos, Amors, and Atens. Various asteroid deflection strategies have been proposed, as early as the 1960s.
The near-Earth asteroid 433 Eros had been discovered as long ago as 1898, and the 1930s brought a flurry of similar objects. In order of discovery, these were: 1221 Amor, 1862 Apollo, 2101 Adonis, and finally 69230 Hermes, which approached within 0.005 AU of Earth in 1937. Astronomers began to realize the possibilities of Earth impact.
Two events in later decades increased the alarm: the increasing acceptance of the Alvarez hypothesis that an impact event resulted in the Cretaceous–Paleogene extinction, and the 1994 observation of Comet Shoemaker-Levy 9 crashing into Jupiter. The U.S. military also declassified the information that its military satellites, built to detect nuclear explosions, had detected hundreds of upper-atmosphere impacts by objects ranging from one to ten meters across.
All these considerations helped spur the launch of highly efficient surveys that consist of charge-coupled device (CCD) cameras and computers directly connected to telescopes. As of 2011[update], it was estimated that 89% to 96% of near-Earth asteroids one kilometer or larger in diameter had been discovered. A list of teams using such systems includes:
As of 29 October 2018[update], the LINEAR system alone has discovered 147,132 asteroids. Among all the surveys, 19,266 near-Earth asteroids have been discovered including almost 900 more than 1 km (0.6 mi) in diameter.
Traditionally, small bodies orbiting the Sun were classified as comets, asteroids, or meteoroids, with anything smaller than one meter across being called a meteoroid. Beech and Steel's 1995 paper proposed a meteoroid definition including size limits. The term "asteroid", from the Greek word for "star-like", never had a formal definition, with the broader term minor planet being preferred by the International Astronomical Union.
However, following the discovery of asteroids below ten meters in size, Rubin and Grossman's 2010 paper revised the previous definition of meteoroid to objects between 10 µm and 1 meter in size in order to maintain the distinction between asteroids and meteoroids. The smallest asteroids discovered (based on absolute magnitude H) are 2008 TS26 with H = 33.2 and 2011 CQ1 with H = 32.1 both with an estimated size of about 1 meter.
In 2006, the term "small Solar System body" was also introduced to cover both most minor planets and comets.[d] Other languages prefer "planetoid" (Greek for "planet-like"), and this term is occasionally used in English especially for larger minor planets such as the dwarf planets as well as an alternative for asteroids since they are not star-like. The word "planetesimal" has a similar meaning, but refers specifically to the small building blocks of the planets that existed when the Solar System was forming. The term "planetule" was coined by the geologist William Daniel Conybeare to describe minor planets, but is not in common use. The three largest objects in the asteroid belt, Ceres, Pallas, and Vesta, grew to the stage of protoplanets. Ceres is a dwarf planet, the only one in the inner Solar System.
When found, asteroids were seen as a class of objects distinct from comets, and there was no unified term for the two until "small Solar System body" was coined in 2006. The main difference between an asteroid and a comet is that a comet shows a coma due to sublimation of near-surface ices by solar radiation. A few objects have ended up being dual-listed because they were first classified as minor planets but later showed evidence of cometary activity. Conversely, some (perhaps all) comets are eventually depleted of their surface volatile ices and become asteroid-like. A further distinction is that comets typically have more eccentric orbits than most asteroids; most "asteroids" with notably eccentric orbits are probably dormant or extinct comets.
For almost two centuries, from the discovery of Ceres in 1801 until the discovery of the first centaur, Chiron in 1977, all known asteroids spent most of their time at or within the orbit of Jupiter, though a few such as Hidalgo ventured far beyond Jupiter for part of their orbit. Those located between the orbits of Mars and Jupiter were known for many years simply as The Asteroids. When astronomers started finding more small bodies that permanently resided further out than Jupiter, now called centaurs, they numbered them among the traditional asteroids, though there was debate over whether they should be considered asteroids or as a new type of object. Then, when the first trans-Neptunian object (other than Pluto), Albion, was discovered in 1992, and especially when large numbers of similar objects started turning up, new terms were invented to sidestep the issue: Kuiper-belt object, trans-Neptunian object, scattered-disc object, and so on. These inhabit the cold outer reaches of the Solar System where ices remain solid and comet-like bodies are not expected to exhibit much cometary activity; if centaurs or trans-Neptunian objects were to venture close to the Sun, their volatile ices would sublimate, and traditional approaches would classify them as comets and not asteroids.
The innermost of these are the Kuiper-belt objects, called "objects" partly to avoid the need to classify them as asteroids or comets. They are thought to be predominantly comet-like in composition, though some may be more akin to asteroids. Furthermore, most do not have the highly eccentric orbits associated with comets, and the ones so far discovered are larger than traditional comet nuclei. (The much more distant Oort cloud is hypothesized to be the main reservoir of dormant comets.) Other recent observations, such as the analysis of the cometary dust collected by the Stardust probe, are increasingly blurring the distinction between comets and asteroids, suggesting "a continuum between asteroids and comets" rather than a sharp dividing line.
The minor planets beyond Jupiter's orbit are sometimes also called "asteroids", especially in popular presentations.[e] However, it is becoming increasingly common for the term "asteroid" to be restricted to minor planets of the inner Solar System. Therefore, this article will restrict itself for the most part to the classical asteroids: objects of the asteroid belt, Jupiter trojans, and near-Earth objects.
When the IAU introduced the class small Solar System bodies in 2006 to include most objects previously classified as minor planets and comets, they created the class of dwarf planets for the largest minor planets – those that have enough mass to have become ellipsoidal under their own gravity. According to the IAU, "the term 'minor planet' may still be used, but generally, the term 'Small Solar System Body' will be preferred." Currently only the largest object in the asteroid belt, Ceres, at about 975 km (606 mi) across, has been placed in the dwarf planet category.
It is thought that planetesimals in the asteroid belt evolved much like the rest of the solar nebula until Jupiter neared its current mass, at which point excitation from orbital resonances with Jupiter ejected over 99% of planetesimals in the belt. Simulations and a discontinuity in spin rate and spectral properties suggest that asteroids larger than approximately 120 km (75 mi) in diameter accreted during that early era, whereas smaller bodies are fragments from collisions between asteroids during or after the Jovian disruption. Ceres and Vesta grew large enough to melt and differentiate, with heavy metallic elements sinking to the core, leaving rocky minerals in the crust.
In the Nice model, many Kuiper-belt objects are captured in the outer asteroid belt, at distances greater than 2.6 AU. Most were later ejected by Jupiter, but those that remained may be the D-type asteroids, and possibly include Ceres.
Distribution within the Solar System
Various dynamical groups of asteroids have been discovered orbiting in the inner Solar System. Their orbits are perturbed by the gravity of other bodies in the Solar System and by the Yarkovsky effect. Significant populations include:
The majority of known asteroids orbit within the asteroid belt between the orbits of Mars and Jupiter, generally in relatively low-eccentricity (i.e. not very elongated) orbits. This belt is now estimated to contain between 1.1 and 1.9 million asteroids larger than 1 km (0.6 mi) in diameter, and millions of smaller ones. These asteroids may be remnants of the protoplanetary disk, and in this region the accretion of planetesimals into planets during the formative period of the Solar System was prevented by large gravitational perturbations by Jupiter.
Trojans are populations that share an orbit with a larger planet or moon, but do not collide with it because they orbit in one of the two Lagrangian points of stability, L4 and L5, which lie 60° ahead of and behind the larger body. The most significant population of trojans are the Jupiter trojans. Although fewer Jupiter trojans have been discovered (as of 2010[update]), it is thought that they are as numerous as the asteroids in the asteroid belt. Trojans have been found in the orbits of other planets, including Venus, Earth, Mars, Uranus, and Neptune.
Near-Earth asteroids, or NEAs, are asteroids that have orbits that pass close to that of Earth. Asteroids that actually cross Earth's orbital path are known as Earth-crossers. As of June 2016[update], 14,464 near-Earth asteroids are known and approximately 900–1,000 have a diameter of over one kilometer.
Asteroids vary greatly in size, from almost 1000 km for the largest down to rocks just 1 meter across.[f] The three largest are very much like miniature planets: they are roughly spherical, have at least partly differentiated interiors, and are thought to be surviving protoplanets. The vast majority, however, are much smaller and are irregularly shaped; they are thought to be either battered planetesimals or fragments of larger bodies.
The dwarf planet Ceres is by far the largest asteroid, with a diameter of 940 km (580 mi). The next largest are 4 Vesta and 2 Pallas, both with diameters of just over 500 km (300 mi). Vesta is the only main-belt asteroid that can, on occasion, be visible to the naked eye. On some rare occasions, a near-Earth asteroid may briefly become visible without technical aid; see 99942 Apophis.
The mass of all the objects of the asteroid belt, lying between the orbits of Mars and Jupiter, is estimated to be in the range of (2.8–3.2)×1021 kg, about 4% of the mass of the Moon. Of this, Ceres comprises 0.938×1021 kg, about a third of the total. Adding in the next three most massive objects, Vesta (9%), Pallas (7%), and Hygiea (3%), brings this figure up to half, whereas the three most-massive asteroids after that, 511 Davida (1.2%), 704 Interamnia (1.0%), and 52 Europa (0.9%), constitute only another 3%. The number of asteroids increases rapidly as their individual masses decrease.
The number of asteroids decreases markedly with size. Although this generally follows a power law, there are 'bumps' at 5 km and 100 km, where more asteroids than expected from a logarithmic distribution are found.
Although their location in the asteroid belt excludes them from planet status, the three largest objects, Ceres, Vesta, and Pallas, are intact protoplanets that share many characteristics common to planets, and are atypical compared to the majority of irregularly shaped asteroids. The fourth-largest asteroid, Hygiea, appears nearly spherical although it may have an undifferentiated interior, like the majority of asteroids. Between them, the four largest asteroids constitute half the mass of the asteroid belt.
Ceres is the only asteroid that appears to be plastic shape under its own gravity and hence the only one that is a likely dwarf planet. It has a much higher absolute magnitude than the other asteroids, of around 3.32, and may possess a surface layer of ice. Like the planets, Ceres is differentiated: it has a crust, a mantle and a core. No meteorites from Ceres have been found on Earth.
Vesta, too, has a differentiated interior, though it formed inside the Solar System's frost line, and so is devoid of water; its composition is mainly of basaltic rock with minerals such as olivine. Aside from the large crater at its southern pole, Rheasilvia, Vesta also has an ellipsoidal shape. Vesta is the parent body of the Vestian family and other V-type asteroids, and is the source of the HED meteorites, which constitute 5% of all meteorites on Earth.
Pallas is unusual in that, like Uranus, it rotates on its side, with its axis of rotation tilted at high angles to its orbital plane. Its composition is similar to that of Ceres: high in carbon and silicon, and perhaps partially differentiated. Pallas is the parent body of the Palladian family of asteroids.
Hygiea is the largest carbonaceous asteroid and, unlike the other largest asteroids, lies relatively close to the plane of the ecliptic. It is the largest member and presumed parent body of the Hygiean family of asteroids. Because there is no sufficiently large crater on the surface to be the source of that family, as there is on Vesta, it is thought that Hygiea may have been completely disrupted in the collision that formed the Hygiean family and recoalesced after losing a bit less than 2% of its mass. Observations taken with the Very Large Telescope's SPHERE imager in 2017 and 2018, and announced in late 2019, revealed that Hygiea has a nearly spherical shape, which is consistent both with it being in hydrostatic equilibrium (and thus a dwarf planet), or formerly being in hydrostatic equilibrium, or with being disrupted and recoalescing.
Measurements of the rotation rates of large asteroids in the asteroid belt show that there is an upper limit. Very few asteroids with a diameter larger than 100 meters have a rotation period smaller than 2.2 hours. For asteroids rotating faster than approximately this rate, the inertial force at the surface is greater than the gravitational force, so any loose surface material would be flung out. However, a solid object should be able to rotate much more rapidly. This suggests that most asteroids with a diameter over 100 meters are rubble piles formed through the accumulation of debris after collisions between asteroids.
The physical composition of asteroids is varied and in most cases poorly understood. Ceres appears to be composed of a rocky core covered by an icy mantle, where Vesta is thought to have a nickel-iron core, olivine mantle, and basaltic crust. 10 Hygiea, however, which appears to have a uniformly primitive composition of carbonaceous chondrite, is thought to be the largest undifferentiated asteroid, though it may be a differentiated asteroid that was globally disrupted by an impact and the reassembled. Other asteroids appear to be the remnant cores or mantles of proto-planets, high in rock and metal Most small asteroids are thought to be piles of rubble held together loosely by gravity, though the largest are probably solid. Some asteroids have moons or are co-orbiting binaries: Rubble piles, moons, binaries, and scattered asteroid families are thought to be the results of collisions that disrupted a parent asteroid, or, possibly, a planet.
In the main asteroid belt, there appear to be two primary populations of asteroid: a dark, volatile-rich population, consisting of the C-type and P-type asteroids, with albedos less that 0.10 and densities under 2.2 g/cm3, and a dense, volatile-poor population, consisting of the S-type and M-type asteroids, with albedos over 0.15 and densities greater than 2.7. Within these populations, larger asteroids are denser, presumably due to compression. There appears to be minimal macro-porosity (interstitial vacuum) in the score of asteroids with masses greater than 10×1018 kg.
Asteroids contain traces of amino acids and other organic compounds, and some speculate that asteroid impacts may have seeded the early Earth with the chemicals necessary to initiate life, or may have even brought life itself to Earth (also see panspermia). In August 2011, a report, based on NASA studies with meteorites found on Earth, was published suggesting DNA and RNA components (adenine, guanine and related organic molecules) may have been formed on asteroids and comets in outer space.
Composition is calculated from three primary sources: albedo, surface spectrum, and density. The last can only be determined accurately by observing the orbits of moons the asteroid might have. So far, every asteroid with moons has turned out to be a rubble pile, a loose conglomeration of rock and metal that may be half empty space by volume. The investigated asteroids are as large as 280 km in diameter, and include 121 Hermione (268×186×183 km), and 87 Sylvia (384×262×232 km). Only half a dozen asteroids are larger than 87 Sylvia, though none of them have moons. The fact that such large asteroids as Sylvia may be rubble piles, presumably due to disruptive impacts, has important consequences for the formation of the Solar System: Computer simulations of collisions involving solid bodies show them destroying each other as often as merging, but colliding rubble piles are more likely to merge. This means that the cores of the planets could have formed relatively quickly.
On 7 October 2009, the presence of water ice was confirmed on the surface of 24 Themis using NASA's Infrared Telescope Facility. The surface of the asteroid appears completely covered in ice. As this ice layer is sublimating, it may be getting replenished by a reservoir of ice under the surface. Organic compounds were also detected on the surface. Scientists hypothesize that some of the first water brought to Earth was delivered by asteroid impacts after the collision that produced the Moon. The presence of ice on 24 Themis supports this theory.
In October 2013, water was detected on an extrasolar body for the first time, on an asteroid orbiting the white dwarf GD 61. On 22 January 2014, European Space Agency (ESA) scientists reported the detection, for the first definitive time, of water vapor on Ceres, the largest object in the asteroid belt. The detection was made by using the far-infrared abilities of the Herschel Space Observatory. The finding is unexpected because comets, not asteroids, are typically considered to "sprout jets and plumes". According to one of the scientists, "The lines are becoming more and more blurred between comets and asteroids."
In May 2016, significant asteroid data arising from the Wide-field Infrared Survey Explorer and NEOWISE missions have been questioned. Although the early original criticism had not undergone peer review, a more recent peer-reviewed study was subsequently published.
In November 2019, scientists reported detecting, for the first time, sugar molecules, including ribose, in meteorites, suggesting that chemical processes on asteroids can produce some fundamentally essential bio-ingredients important to life, and supporting the notion of an RNA world prior to a DNA-based origin of life on Earth, and possibly, as well, the notion of panspermia.
Findings have shown that solar winds can react with the oxygen in the upper layer of the asteroids and create water. It has been estimated that every cubic metre of irradiated rock could contain up to 20 litres.
Most asteroids outside the "big four" (Ceres, Pallas, Vesta, and Hygiea) are likely to be broadly similar in appearance, if irregular in shape. 50 km (31 mi) 253 Mathilde is a rubble pile saturated with craters with diameters the size of the asteroid's radius, and Earth-based observations of 300 km (186 mi) 511 Davida, one of the largest asteroids after the big four, reveal a similarly angular profile, suggesting it is also saturated with radius-size craters. Medium-sized asteroids such as Mathilde and 243 Ida that have been observed up close also reveal a deep regolith covering the surface. Of the big four, Pallas and Hygiea are practically unknown. Vesta has compression fractures encircling a radius-size crater at its south pole but is otherwise a spheroid. Ceres seems quite different in the glimpses Hubble has provided, with surface features that are unlikely to be due to simple craters and impact basins, but details will be expanded with the Dawn spacecraft, which entered Ceres orbit on 6 March 2015.
Asteroids become darker and redder with age due to space weathering. However evidence suggests most of the color change occurs rapidly, in the first hundred thousand years, limiting the usefulness of spectral measurement for determining the age of asteroids.
Asteroids are commonly categorized according to two criteria: the characteristics of their orbits, and features of their reflectance spectrum.
Many asteroids have been placed in groups and families based on their orbital characteristics. Apart from the broadest divisions, it is customary to name a group of asteroids after the first member of that group to be discovered. Groups are relatively loose dynamical associations, whereas families are tighter and result from the catastrophic break-up of a large parent asteroid sometime in the past. Families are more common and easier to identify within the main asteroid belt, but several small families have been reported among the Jupiter trojans. Main belt families were first recognized by Kiyotsugu Hirayama in 1918 and are often called Hirayama families in his honor.
About 30–35% of the bodies in the asteroid belt belong to dynamical families each thought to have a common origin in a past collision between asteroids. A family has also been associated with the plutoid dwarf planet Haumea.
Quasi-satellites and horseshoe objects
Some asteroids have unusual horseshoe orbits that are co-orbital with Earth or some other planet. Examples are 3753 Cruithne and 2002 AA29. The first instance of this type of orbital arrangement was discovered between Saturn's moons Epimetheus and Janus.
Sometimes these horseshoe objects temporarily become quasi-satellites for a few decades or a few hundred years, before returning to their earlier status. Both Earth and Venus are known to have quasi-satellites.
In 1975, an asteroid taxonomic system based on color, albedo, and spectral shape was developed by Chapman, Morrison, and Zellner. These properties are thought to correspond to the composition of the asteroid's surface material. The original classification system had three categories: C-types for dark carbonaceous objects (75% of known asteroids), S-types for stony (silicaceous) objects (17% of known asteroids) and U for those that did not fit into either C or S. This classification has since been expanded to include many other asteroid types. The number of types continues to grow as more asteroids are studied.
The two most widely used taxonomies now used are the Tholen classification and SMASS classification. The former was proposed in 1984 by David J. Tholen, and was based on data collected from an eight-color asteroid survey performed in the 1980s. This resulted in 14 asteroid categories. In 2002, the Small Main-Belt Asteroid Spectroscopic Survey resulted in a modified version of the Tholen taxonomy with 24 different types. Both systems have three broad categories of C, S, and X asteroids, where X consists of mostly metallic asteroids, such as the M-type. There are also several smaller classes.
The proportion of known asteroids falling into the various spectral types does not necessarily reflect the proportion of all asteroids that are of that type; some types are easier to detect than others, biasing the totals.
Originally, spectral designations were based on inferences of an asteroid's composition. However, the correspondence between spectral class and composition is not always very good, and a variety of classifications are in use. This has led to significant confusion. Although asteroids of different spectral classifications are likely to be composed of different materials, there are no assurances that asteroids within the same taxonomic class are composed of the same (or similar) materials.
A newly discovered asteroid is given a provisional designation (such as 2002 AT4) consisting of the year of discovery and an alphanumeric code indicating the half-month of discovery and the sequence within that half-month. Once an asteroid's orbit has been confirmed, it is given a number, and later may also be given a name (e.g. 433 Eros). The formal naming convention uses parentheses around the number – e.g. (433) Eros – but dropping the parentheses is quite common. Informally, it is common to drop the number altogether, or to drop it after the first mention when a name is repeated in running text. In addition, names can be proposed by the asteroid's discoverer, within guidelines established by the International Astronomical Union.
The first asteroids to be discovered were assigned iconic symbols like the ones traditionally used to designate the planets. By 1855 there were two dozen asteroid symbols, which often occurred in multiple variants.
In 1851, after the fifteenth asteroid (Eunomia) had been discovered, Johann Franz Encke made a major change in the upcoming 1854 edition of the Berliner Astronomisches Jahrbuch (BAJ, Berlin Astronomical Yearbook). He introduced a disk (circle), a traditional symbol for a star, as the generic symbol for an asteroid. The circle was then numbered in order of discovery to indicate a specific asteroid (although he assigned ① to the fifth, Astraea, while continuing to designate the first four only with their existing iconic symbols). The numbered-circle convention was quickly adopted by astronomers, and the next asteroid to be discovered (16 Psyche, in 1852) was the first to be designated in that way at the time of its discovery. However, Psyche was given an iconic symbol as well, as were a few other asteroids discovered over the next few years (see chart above). 20 Massalia was the first asteroid that was not assigned an iconic symbol, and no iconic symbols were created after the 1855 discovery of 37 Fides.[h] That year Astraea's number was increased to ⑤, but the first four asteroids, Ceres to Vesta, were not listed by their numbers until the 1867 edition. The circle was soon abbreviated to a pair of parentheses, which were easier to typeset and sometimes omitted altogether over the next few decades, leading to the modern convention.
Until the age of space travel, objects in the asteroid belt were merely pinpricks of light in even the largest telescopes and their shapes and terrain remained a mystery. The best modern ground-based telescopes and the Earth-orbiting Hubble Space Telescope can resolve a small amount of detail on the surfaces of the largest asteroids, but even these mostly remain little more than fuzzy blobs. Limited information about the shapes and compositions of asteroids can be inferred from their light curves (their variation in brightness as they rotate) and their spectral properties, and asteroid sizes can be estimated by timing the lengths of star occultations (when an asteroid passes directly in front of a star). Radar imaging can yield good information about asteroid shapes and orbital and rotational parameters, especially for near-Earth asteroids. In terms of delta-v and propellant requirements, NEOs are more easily accessible than the Moon.
The first close-up photographs of asteroid-like objects were taken in 1971, when the Mariner 9 probe imaged Phobos and Deimos, the two small moons of Mars, which are probably captured asteroids. These images revealed the irregular, potato-like shapes of most asteroids, as did later images from the Voyager probes of the small moons of the gas giants.
In September 2007, NASA launched the Dawn spacecraft, which orbited 4 Vesta from July 2011 to September 2012, and has been orbiting the dwarf planet 1 Ceres since 2015. 4 Vesta is the second-largest asteroid visited to date.
In June 2018, the US National Science and Technology Council warned that America is unprepared for an asteroid impact event, and has developed and released the "National Near-Earth Object Preparedness Strategy Action Plan" to better prepare.
In September 2016, NASA launched the OSIRIS-REx sample return mission to asteroid 101955 Bennu, which it reached in December 2018. On May 10 2021, the probe departed the asteroid with a sample from its surface, and is expected to return to Earth on September 24 2023.
Planned and future missions
In early 2013, NASA announced the planning stages of a mission to capture a near-Earth asteroid and move it into lunar orbit where it could possibly be visited by astronauts and later impacted into the Moon. On 19 June 2014, NASA reported that asteroid 2011 MD was a prime candidate for capture by a robotic mission, perhaps in the early 2020s.
It has been suggested that asteroids might be used as a source of materials that may be rare or exhausted on Earth (asteroid mining), or materials for constructing space habitats (see Colonization of the asteroids). Materials that are heavy and expensive to launch from Earth may someday be mined from asteroids and used for space manufacturing and construction.
In November 2021, NASA launched its Double Asteroid Redirection Test (DART), a mission to test technology for defending Earth against potential asteroids or comets.
Location of Ceres (within asteroid belt) compared to other bodies of the Solar System
Asteroids and the asteroid belt are a staple of science fiction stories. Asteroids play several potential roles in science fiction: as places human beings might colonize, resources for extracting minerals, hazards encountered by spacecraft traveling between two other points, and as a threat to life on Earth or other inhabited planets, dwarf planets, and natural satellites by potential impact.
Further information about asteroids