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Lista de objetos del Sistema Solar por tamaño

Diagrama de partes por millón de la distribución de masa relativa del Sistema Solar, donde cada cubo representa 2 × 1024  kilos

Este artículo incluye una lista de los objetos más masivos conocidos del Sistema Solar y listas parciales de objetos más pequeños según el radio medio observado . Estas listas se pueden ordenar según el radio y la masa del objeto y, en el caso de los objetos más masivos, según el volumen, la densidad y la gravedad superficial, si estos valores están disponibles.

Estas listas contienen el Sol , los planetas , los planetas enanos , muchos de los cuerpos pequeños más grandes del Sistema Solar (que incluye los asteroides ), todos los satélites naturales nombrados y una serie de objetos más pequeños de interés histórico o científico, como cometas y objetos cercanos a la Tierra .

Se han descubierto muchos objetos transneptunianos (TNO); en muchos casos sus posiciones en esta lista son aproximadas, ya que con frecuencia existe una gran incertidumbre en sus diámetros estimados debido a su distancia de la Tierra.

Se sabe o se espera que los objetos del Sistema Solar con una masa superior a 10 21 kilogramos sean aproximadamente esféricos. Los cuerpos astronómicos se relajan hasta adoptar formas redondeadas ( esferoides ), alcanzando el equilibrio hidrostático , cuando su propia gravedad es suficiente para superar la resistencia estructural de su material. Se creía que el límite para los objetos redondos está entre 100 km y 200 km de radio si tienen una gran cantidad de hielo en su composición; [1] sin embargo, estudios posteriores revelaron que los satélites helados tan grandes como Jápeto (1.470 kilómetros de diámetro) no están en equilibrio hidrostático en este momento, [2] y una evaluación de 2019 sugiere que muchos TNO en el rango de tamaño de 400 a 1.000 kilómetros pueden ni siquiera ser cuerpos completamente sólidos, mucho menos redondeados gravitacionalmente. [3] Los objetos que son elipsoides debido a su propia gravedad se denominan aquí generalmente "redondos", independientemente de que estén o no en equilibrio en la actualidad, mientras que los objetos que claramente no son elipsoidales se denominan "irregulares".

Los cuerpos esferoidales suelen tener cierto aplanamiento polar debido a la fuerza centrífuga de su rotación y, a veces, incluso pueden tener diámetros ecuatoriales bastante diferentes ( elipsoides escalenos como Haumea ). A diferencia de cuerpos como Haumea, los cuerpos irregulares tienen un perfil significativamente no elipsoidal, a menudo con bordes afilados.

Puede resultar difícil determinar el diámetro (con un margen de error de aproximadamente 2) de los objetos típicos situados más allá de Saturno (véase 2060 Chiron como ejemplo). En el caso de los TNO, hay cierta confianza en los diámetros, pero en el caso de los TNO no binarios no hay una confianza real en las masas/densidades. A menudo se supone que muchos TNO tienen la densidad de Plutón de 2,0 g/cm 3 , pero es igualmente probable que tengan una densidad similar a la de un cometa de solo 0,5 g/cm 3 . [4]

Por ejemplo, si se supone incorrectamente que un TNO tiene una masa de 3,59 × 1020 kg basado en un radio de 350 km con una densidad de 2 g/cm 3 pero luego se descubre que tiene un radio de solo 175 km con una densidad de 0,5 g/cm 3 , su masa real sería solo 1,12 × 1019 kilos.

Los tamaños y masas de muchas de las lunas de Júpiter y Saturno son bastante conocidos debido a numerosas observaciones e interacciones de los orbitadores Galileo y Cassini ; sin embargo, muchas de las lunas con un radio menor a ~100 km, como Himalia de Júpiter , tienen masas mucho menos seguras. [5] Más allá de Saturno, los tamaños y masas de los objetos son menos claros. Todavía no ha habido un orbitador alrededor de Urano o Neptuno para el estudio a largo plazo de sus lunas. Para las pequeñas lunas irregulares exteriores de Urano, como Sycorax , que no fueron descubiertas por el sobrevuelo de la Voyager 2 , incluso diferentes páginas web de la NASA, como el Centro Nacional de Datos de Ciencias Espaciales [6] y JPL Solar System Dynamics, [5] dan estimaciones de tamaño y albedo algo contradictorias según el artículo de investigación que se cite.

Existen incertidumbres en las cifras de masa y radio, e irregularidades en la forma y densidad; la precisión a menudo depende de lo cerca que esté el objeto de la Tierra o de si ha sido visitado por una sonda.

Visión general gráfica

Diámetros relativos de los cincuenta cuerpos más grandes del Sistema Solar, coloreados por región orbital. Los valores son diámetros en kilómetros. La escala es lineal.

Objetos con radios superiores a 400 km

Los siguientes objetos tienen un radio medio de al menos 400 km. En un principio se esperaba que cualquier cuerpo helado con un radio superior a los 200 km estuviera en equilibrio hidrostático (HE). [7] Sin embargo, Ceres (r = 470 km) es el cuerpo más pequeño para el que las mediciones detalladas son consistentes con el equilibrio hidrostático, [8] mientras que Jápeto (r = 735 km) es el cuerpo helado más grande que se ha descubierto que no está en equilibrio hidrostático. [9] Las lunas heladas conocidas en este rango son todas elipsoidales (excepto Proteo ), pero los objetos transneptunianos de hasta 450–500 km de radio pueden ser bastante porosos. [10]

Para simplificar y hacer comparaciones, los valores se calculan manualmente asumiendo que todos los cuerpos son esferas. El tamaño de los cuerpos sólidos no incluye la atmósfera del objeto. Por ejemplo, Titán parece más grande que Ganimedes, pero su cuerpo sólido es más pequeño. Para los planetas gigantes , el "radio" se define como la distancia desde el centro en la que la atmósfera alcanza 1 bar de presión atmosférica. [11]

Dado que Sedna y 2002 MS 4 no tienen lunas conocidas, determinar directamente su masa es imposible sin enviar una sonda (se estima que va de 1,7x10 21 a 6,1×10 21 kg para Sedna [12] ).

Objetos más pequeños por radio medio

De 200 a 399 km

Todas las lunas heladas fotografiadas con radios mayores de 200 km, excepto Proteus, son claramente redondas, aunque aquellas de menos de 400 km cuyas formas se han medido cuidadosamente no están en equilibrio hidrostático. [58] Las densidades conocidas de TNO en este rango de tamaño son notablemente bajas (1–1,2 g/cm 3 ), lo que implica que los objetos conservan una porosidad interna significativa desde su formación y nunca fueron comprimidos gravitacionalmente hasta convertirse en cuerpos completamente sólidos. [10]

De 100 a 199 km

Esta lista contiene una selección de objetos cuyo radio se estima entre 100 y 199 km (200 y 399 km de diámetro). Los más grandes de ellos pueden tener una forma de equilibrio hidrostático, pero la mayoría son irregulares. La mayoría de los objetos transneptunianos (TNO) enumerados con un radio menor de 200 km tienen " tamaños asumidos basados ​​en un albedo genérico de 0,09" ya que están demasiado lejos para medir directamente sus tamaños con los instrumentos existentes. La masa varía de 10 21 kg a 10 18 kg (Zg). Los asteroides del cinturón principal tienen elementos orbitales restringidos por (2,0 UA < a < 3,2 UA; q > 1,666 UA) según JPL Solar System Dynamics (JPLSSD). [100] Muchos TNO se omiten de esta lista porque sus tamaños son poco conocidos. [59]

De 50 a 99 km

Esta lista contiene una selección de objetos de 50 y 99 km de radio (de 100 km a 199 km de diámetro medio). Los objetos enumerados actualmente incluyen la mayoría de los objetos del cinturón de asteroides y las lunas de los planetas gigantes en este rango de tamaño, pero faltan muchos objetos recién descubiertos en el Sistema Solar exterior, como los incluidos en la siguiente referencia. [59] Los tipos espectrales de asteroides son en su mayoría Tholen, pero algunos podrían ser SMASS.

De 20 a 49 km

Esta lista incluye pocos ejemplos, ya que hay alrededor de 589 asteroides en el cinturón de asteroides con un radio medido entre 20 y 49 km. [162] Muchos miles de objetos de este rango de tamaño aún no se han descubierto en la región transneptuniana. El número de dígitos no es una aprobación de cifras significativas . La tabla cambia de × 1018  kg a × 1015  kg ( Eg ). Se suponen la mayoría de los valores de masa de los asteroides. [114] [163]

De 1 a 19 km

Esta lista contiene algunos ejemplos de objetos del Sistema Solar con un radio de entre 1 y 19 km. Este es un tamaño común para asteroides, cometas y lunas irregulares.

Below 1 km

This list contains examples of objects below 1 km in radius. That means that irregular bodies can have a longer chord in some directions, hence the mean radius averages out. In the asteroid belt alone there are estimated to be between 1.1 and 1.9 million objects with a radius above 0.5 km,[246] many of which are in the range 0.5–1.0 km. Countless more have a radius below 0.5 km. Very few objects in this size range have been explored or even imaged. The exceptions are objects that have been visited by a probe, or have passed close enough to Earth to be imaged. Radius is by mean geometric radius. Number of digits not an endorsement of significant figures. Mass scale shifts from × 1015 to 109 kg, which is equivalent to one billion kg or 1012 grams (Teragram – Tg). Currently most of the objects of mass between 109 kg to 1012 kg (less than 1000 teragrams (Tg)) listed here are near-Earth asteroids (NEAs). The Aten asteroid 1994 WR12 has less mass than the Great Pyramid of Giza, 5.9 × 109 kg. For more about very small objects in the Solar System, see meteoroid, micrometeoroid, cosmic dust, and interplanetary dust cloud. (See also Visited/imaged bodies.)

Gallery

Solar system planets, major moons, and 3 stars of different sizes are shown comparatively in three levels of zoom: one for the rocky planets, one for the gas giants, and one for the stars.
Largest moons of the Solar System to scale.

See also

Notes

  1. ^ a b c d e Radius estimated using equatorial radius and assuming body is spherical
  2. ^ a b Radius has been determined by various methods, such as optical (Hubble), thermal (Spitzer), or direct imaging via spacecraft
  3. ^ Calculated in Wolfram Alpha using semi axes of 1050 × 840 × 537 (Ellipsoid volume: 1.98395×10^9 km3)
  4. ^ Best fit, assuming Haumea is in hydrostatic equilibrium
  5. ^ a b c Radius estimated by using three radii and assuming body is spheroid
  6. ^ The mass estimate is based on the assumed density of 1.2 g/cm3, and a volume of 3.5 ×106 km3 obtained from a detailed shape model in Stooke (1994).[120]
  1. ^ a b c d e f g Name of body, including alternative names using Roman numerals to designate moons (such as "Saturn I" for Mimas), and numbers to designate minor planets
  2. ^ a b c d e f g Mean radius including uncertainties
  3. ^ Given as surface gravity (1 bar for gaseous planets)
  4. ^ Figures from default source Johnston's Archive—List of Known Trans-Neptunian Objects,[59] if otherwise not mentioned in the References column
  5. ^ a b c d e f Reference column specifically for radius (r) and mass (M) citations

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Further reading

External links