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Product Name: KX1908 Space Instrument (Three-Ball Instrument)
Model Number: KX1908
Size: 120*120*110 mm
Weight: Approximately 150g
Material: wood + battery case + reduction motor + shaft + foam balls...
Packaging: 200 pcs
Box dimensions: 600*550*450 mm
Note: The product is in natural wood color, and the color on it was painted with acrylic paint, which needs to be purchased separately.

The model of the operating laws among the sun, Earth, and Moon is the trisphere.
The Earth-Moon-Sun motion demonstration model is a simple three-ball instrument toy that serves as an intuitive teaching model to vividly illustrate the relative movement between the Earth, Moon, and Sun.
Children can use their hands to make the Earth, Moon, and Sun in the model move according to real-world laws of motion, which is very interesting!

The trisphere instrument consists of three small spheres representing the sun, Earth, and Moon, along with mechanical linkage mechanisms, which are used to demonstrate the relationships among these three bodies and some astronomical phenomena resulting from them. To mimic real-world conditions, the central sun is typically represented by a light bulb that illuminates Earth and the Moon. Earth rotates obliquely around the sun in its orbit, and the orbit of the Moon around Earth intersects with Earth’s orbit around the sun at a certain angle. This allows for the demonstration of phenomena such as solar eclipses and lunar eclipses, the phases of the Moon, Earth’s rotation and revolution, as well as the alternation of day and night and the seasons.
The purpose of this utility model is to provide a Earth-Moon system operating model that not only objectively reflects the spatial positions of the sun, Earth, and moon, but also visually and systematically demonstrates the movements of these celestial bodies, as well as various natural phenomena resulting from their mutual motion.
The Earth rotates around the Sun, completing one orbit in about 365 days; the Moon rotates around the Earth, also completing one orbit in about 365 days. Moreover, both of them have their own rotation.

A lunar eclipse is a special astronomical phenomenon where, when the moon moves into the Earth's shadow, the area between the moon and Earth is obscured by the Earth, causing the moon to appear partially missing. At this time, the sun, Earth, and moon are exactly (or almost) in a straight line. Lunar eclipses can be divided into partial, total, and penumbral types. Lunar eclipses can only occur around the 15th day of the lunar month.
A shadow appears on the side of the Earth away from the sun, known as the umbra. The umbra is divided into two parts: the penumbra and the antumbra. The penumbra refers to areas not directly exposed to sunlight, while the antumbra receives only partially direct sunlight. The Moon sometimes enters the umbra during its orbit around the Earth, resulting in a lunar eclipse. When the entire Moon enters the umbra, a total lunar eclipse occurs; if only a portion enters the umbra, then a partial lunar eclipse takes place. Both total and partial lunar eclipses are types of umbral eclipses.
Eclipses can be divided into three types: partial eclipse, total eclipse, and penumbral eclipse. A partial eclipse occurs when only part of the Moon enters Earth's umbra; this happens when the diameter of Earth's umbra is approximately 2.5 times that of the Moon, ensuring the centers of Earth and the Moon are roughly on the same line, allowing the Moon to fully enter the umbra and result in a total eclipse. In contrast, a partial eclipse occurs when only part of the Moon is covered by Earth's umbra—i.e., only a portion of the umbra covers the Moon. A lunar ring eclipse does not occur because the Moon is smaller than Earth, and thus there is no area within Earth's umbra where a lunar ring phenomenon could take place. Eclipses generally occur two times per year, sometimes three times, and occasionally not at all. Under normal circumstances, the Moon either passes above or below Earth's umbra, rarely passing through or partially passing through the umbra, so eclipses do not occur frequently. According to observational data, the percentages of penumbral eclipses, partial eclipses, and total eclipses per century are approximately 36.6%, 34.46%, and 28.94%, respectively.
The penumbral phase begins during the partial eclipse: the moon just touches the penumbra, which is imperceptible to the naked eye. The full lunar eclipse process consists of five stages: first contact, beginning of obscuration, peak obscuration, emergence of light, and full restoration.
Penumbral ingestion begins: The moon just touches the penumbral region, at which point the brightness on the lunar surface slightly decreases, though it is difficult to detect with the naked eye.
First eclipse (only lunar partial and total eclipses): Indicates the start of a lunar eclipse. The Moon slowly enters the Earth's shadow from the eastern edge, with the Moon and the Earth's umbra being nearly tangent.
Eclipse of the Moon (only lunar eclipse): The moon enters the Earth's umbra and is tangent to it. The moon completely enters the Earth's umbra.
Food Time: At the moment when the center of the full moon approaches the center of the Earth's shadow, the surface of the Moon appears copper-red or dark red. (Reason: Sunlight refracts as it passes through the Earth's atmosphere, bending inward, and the degree of refraction varies for different colors (dispersion). Red light is more refracted, approaching the Earth's shadow, and appears on the Moon; additionally, due to differences in dust and cloud content and location in the atmosphere, the refraction varies, resulting in the Moon appearing dark red, copper-red, or orange during a total solar eclipse. Similarly, due to atmospheric refraction, sunrise and sunset are not white, and depending on altitude, they appear orange or red.)
Shengguang (total lunar eclipse only): The moon moves within the Earth's umbra and forms a second contact with it. When the eastern edge of the moon touches the eastern edge of the Earth's umbra, the total eclipse phase ends.
Partial and total lunar eclipses (only lunar eclipse and lunar eclipse): The Moon gradually moves away from the Earth's umbra, reaching a second contact with it. When the western edge of the Moon touches the eastern edge of the Earth's umbra, the entire lunar eclipse is complete. The degree to which the Moon is eclipsed is called "eclipse magnitude," which equals the ratio of the distance at which the Moon's edge enters the Earth's umbra during the peak of the eclipse to the Moon's apparent path.
Penumbral eclipse end: The moon exits the penumbra, marking the official conclusion of the entire eclipse event. There is no eclipse bite or brilliance phase during a lunar partial eclipse, and the peak of the eclipse only indicates the moment when the moon approaches the Earth's shadow.
The extent of a lunar eclipse is expressed as the eclipse fraction. The eclipse fraction is equal to the ratio of the part of the lunar apparent diameter that enters the umbra during the maximum eclipse to the total lunar apparent diameter. If the moon touches the edge of the umbra during the maximum eclipse, the eclipse fraction is 1. If the moon enters the umbra further, the eclipse fraction is represented by a number greater than 1. The eclipse fraction for a total lunar eclipse is greater than or equal to 1. For partial eclipses, the eclipse fraction is less than 1. For penumbral lunar eclipses, the eclipse fraction is expressed as the ratio of the part of the lunar diameter that enters the penumbra to the lunar apparent diameter. A penumbral lunar eclipse can be detected with the naked eye only when the eclipse fraction is greater than 0.7.