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Ada beberapa pertanyaan yang jelas terkait dengan Tata Surya. Yang
pertama mungkin `` berapa lama itu?'' Teori evolusi Stellar mengatakan
bahwa Sun sekitar 5 miliar tahun, tapi itu tergantung pada seberapa
baik kita memahami bagaimana bintang bekerja
Nicolaus Copernicus; Tokoh Heliosentris
(1473-1543)
Immanuel Kant (1724-1804)
Nebular Hypothesis:
A second theory is called the nebular hypothesis. In this theory, the
whole Solar System starts as a large cloud of gas that contracts under
self-gravity. Conservation of angular momentum requires that a
rotating disk form with a large concentration at the center (the protoSun). Within the disk, planets form.
Adanya Kabut Nebula
Kabut itu berputar dengan kuat &
terjadi pemadatan di bagian tengah
Di bagian tengah terbentuk Matahari
dan di pinggirnya terbentuk planetplanet
Planet-planet terus berputar dan
membentuk orbit mengelilingi
Matahari
Maka terbentuklah Tata Surya
Gerald P. Kuiper
(1905-1973)
Protoplanet Hypothesis:
The current working model for the formation of the Solar System is
called the protoplanet hypothesis. It incorporates many of the
components of the nebular hypothesis, but adds some new aspects
from modern knowledge of fluids and states of matter.
Teori Kuiper:
-Semesta terdiri dari formasi debu kosmik
-Dua pusat memadat menjadi dua bintang, terdiri dari hidrogen
-Pusat yang lebih besar memadat menjadi bintang tunggal
-Bagian yang lebih kecil menjadi material Protoplanet
-Protoplanet tersebut kemudian menjadi planet
-Jika kekuatan dua bintang itu sama, maka akan terbentuk
bintang ganda/kembar
How did the Solar System form? Any theory of the solar
system formation must account for the obvious features we
see, such as 1) the fact that solar system is a fairly flat place,
with all the planets within a few degrees of the ecliptic and
revolving in roughly circular oribts that are all going in the
same direction, 2) the division between the small, rocky
terrestrial planets in the inner part of the solar system, and the
hydrogen-rich Jovian planets in the outer solar system, 3) the
decrease in average planet density from the inner part of the
solar system to the outer part, and 4) the existence of Bodes
law, with each planet roughly twice as far from the Sun as the
previous planet.
Thomas Chrowder Chamberline
(1843-1928)
There was encounter between the Sun and another star. In this
scenario, the gravity of the passing star tears a succession of bolts
from the solar surface. Bolts coming from the side nearer the star are
thrown out to distances comparable with those of the giant plants,
while those from the far side of the Sun are ejected less violently to
the distances of the terrestrial planets. From the inner remains of
these bolts formed the initial cores of the planets. The outer parts
expanded and cooled into a huge swarm of solid particles spread out
in a disk rotating about the Sun in a plane determined by the motion of
the passing star. The cores gradually grew into planets by gathering in
the planetesimals, most of the growth taking place in the outer parts of
the Solar System where material was more plentiful. Eventually it
became clear that, like other variants of the encounter idea, not
enough angular momentum could be conveyed to the ejected material
to explain the state of the Solar System as it exists today.
James Jeans
(1877-1946)
Encounter Hypothesis:
One of the earliest theories for the formation of the planets was
called the encounter hypothesis. In this scenario, a rogue star
passes close to the Sun about 5 billion years ago. Material, in the
form of hot gas, is tidally stripped from the Sun and the rogue star.
This material fragments into smaller lumps which form the planets.
This hypothesis has the advantage of explaining why the planets all
revolve in the same direction (from the encounter geometry) and also
provides an explanation for why the inner worlds are denser than the
outer worlds.
Pertemuan 2 bintang…
Susunan planet-planet seperti cerutu: kecil pada
kedua ujungnya & besar di bagian tengahnya
Komar©November 2008