Orbit and rotation of Gyrd
Overview
Like how real-life Earth orbits around the real-life Sun, Gyrd (English pronunciation: GEERD) orbits around Hysb, and, like how real-life Earth rotates on its own axis, Gyrd rotates on its own axis. Gyrd is the third planet from Hysb and the only planet that orbits Hysb that is within Hysb's circumstellar habitable zone, and Gyrd takes a longer amount of time to both complete one orbit around Hysb than real-life Earth does to orbit the real-life Sun and complete one rotation on its own axis than real-life Earth.
Synodic orbit of Gyrd
Gyrd's synodic orbit is its path around Hysb, the star that it orbits, relative to the barycenter of the orbit around Gyrd and Hysb, which is located within Hysb. Gyrd's orbit is influenced greatly by the orbit of Hysb and Zorl around their common barycenter, which takes seven and a half times as long as Gyrd's synodic orbit around Hysb. As a result, Gyrd can be thought of as having both a synodic orbit and a quattoural cycle.
Gyrd's mean orbital distance from Hysb is approximately 242,000,000 kilometers from barycenter of Gyrd's orbit around Hysb. Two factors prevent Gyrd from having a perfectly circular orbit. One factor that prohibits Gyrd from having a perfectly circular orbit is the fact that Gyrd's synodic orbit is somewhat octagonal in shape. Gyrd is closer to the barycenter of its orbit around Hysb at each solstice, at each equinox, and at the midpoint between any solstice or equinox and the following solstice or equinox than at any adjacent midpoint between a solstice or equinox and either adjacent midpoint between a solstice and an equinox. Because of the octagonal nature of Gyrd's synodic orbit, Gyrd can be thought of has having eight minor perihelions and eight minor aphelions each synodic year. The other factor that prohibits Gyrd from having a perfectly circular orbit is the quattoural cycle, fourteen Gyrdian synodic years in length, caused by Hysb and Zorl orbiting a common barycenter. Gyrd can be thought of as having two major aphelions and four major perihelions during each quattoural cycle. At the equinox three and three-quarter Gyrdian synodic years, and at the equinox eleven and one-quarter Gyrdian synodic years, following the solstice that begins the quattoural cycle, which is a winter solstice in Gyrd's northern hemisphere, Gyrd is at major perihelion, or the closest that Gyrd comes to Hysb at any point in a seven and one-half Gyrdian year period. At each minor aphelion either preceding or following the midpoint of a quattoral cycle and at each minor aphelion preceding the solstice that begins a new quattoural cycle, Gyrd is at major aphelion, or the furthest Gyrd comes to Hysb at any point in a seven and one-half Gyrdian year period. While, due to the quattoural cycle, neither minor perihelions nor minor aphelions are of uniform distance between Gyrd and Hysb, Gyrd is approximately 236,000,000 kilometers from the barycenter of Gyrd's orbit around Hysb at major perihelion and approximately 248,000,000 kilometers from the barycenter of Gyrd's orbit around Hysb at major aphelion. This puts Gyrd's orbit wholly within the outer half of Harb's circumstellar habitable zone.
As viewed from Gyrd's north geographical pole, Gyrd rotates in an anticlockwise direction. The inclination, or the orbital tilt, of Gyrd's synodic orbit relative to Hysb's equator is approximately five degrees. As Hysb appears as a disk, not a point, of light from Gyrd, and the inclination of the orbits of Hysb and Zorl relative to the invariable plane of the barycenter that Hysb and Zorl orbit are each approximately zero degrees, A total binary eclipse of Zorl by Hysb as viewed from Gyrd occurs every seven and one-half Gyrdian years.
The mean Gyrdian synodic year within any quattoral cycle is 472.2475 mean Gyrdian synodic days in length. In years in which Gyrd has a major perihelion, the Gyrdian synodic year is approximately 472.24 mean Gyrdian synodic days in length. In years in which Gyrd has a major aphelion, the Gyrdian synodic year is approximately 472.255 mean Gyrdian synodic days in length. Due to Gyrd's rotation, which is explained in more detail in the following section of this page, the Gyrdian synodic day is noticeably longer than real-life Earth's synodic day, with the mean Gyrdian synodic year measuring approximately 590.3094 Earth days in length.
Synodic rotation of Gyrd
Gyrd's synodic rotation is the rotation on its own axis relative to Hysb.
One complete rotation by Gyrd on its own axis relative to Hysb is known as a Gyrdian synodic day. The mean Gyrdian synodic day is roughly 30 Earth hours in length. There is a slight variance in the length of each Gyrdian synodic day due to Gyrd's orbit being non-circular, as well as Gyrd not having a completely consistent rotational speed. The difference between the length of Gyrd's synodic day when Gyrd is at major perihelion than the length of Gyrd's synodic day when Gyrd is at major aphelion is approximately four Earth seconds in length. The Gyrdian synodic day is at its longest when Gyrd is at major aphelion and at its shortest when Gyrd is at major perihelion.
Gyrd rotates on its own axis in an anticlockwise direction, as viewed from above Gyrd's north geographical pole. Gyrd's axial tilt, or the angle of Gyrd's axis of rotation relative to the plane of Gyrd's synodic orbit, is approximately 22.5 degrees, which is slightly less than that of real-life Earth. Gyrd's axial tilt is one of several factors contributing to Gyrd's climate patterns and meteorological seasons.
Like how real-life Earth orbits around the real-life Sun, Gyrd (English pronunciation: GEERD) orbits around Hysb, and, like how real-life Earth rotates on its own axis, Gyrd rotates on its own axis. Gyrd is the third planet from Hysb and the only planet that orbits Hysb that is within Hysb's circumstellar habitable zone, and Gyrd takes a longer amount of time to both complete one orbit around Hysb than real-life Earth does to orbit the real-life Sun and complete one rotation on its own axis than real-life Earth.
Synodic orbit of Gyrd
Gyrd's synodic orbit is its path around Hysb, the star that it orbits, relative to the barycenter of the orbit around Gyrd and Hysb, which is located within Hysb. Gyrd's orbit is influenced greatly by the orbit of Hysb and Zorl around their common barycenter, which takes seven and a half times as long as Gyrd's synodic orbit around Hysb. As a result, Gyrd can be thought of as having both a synodic orbit and a quattoural cycle.
Gyrd's mean orbital distance from Hysb is approximately 242,000,000 kilometers from barycenter of Gyrd's orbit around Hysb. Two factors prevent Gyrd from having a perfectly circular orbit. One factor that prohibits Gyrd from having a perfectly circular orbit is the fact that Gyrd's synodic orbit is somewhat octagonal in shape. Gyrd is closer to the barycenter of its orbit around Hysb at each solstice, at each equinox, and at the midpoint between any solstice or equinox and the following solstice or equinox than at any adjacent midpoint between a solstice or equinox and either adjacent midpoint between a solstice and an equinox. Because of the octagonal nature of Gyrd's synodic orbit, Gyrd can be thought of has having eight minor perihelions and eight minor aphelions each synodic year. The other factor that prohibits Gyrd from having a perfectly circular orbit is the quattoural cycle, fourteen Gyrdian synodic years in length, caused by Hysb and Zorl orbiting a common barycenter. Gyrd can be thought of as having two major aphelions and four major perihelions during each quattoural cycle. At the equinox three and three-quarter Gyrdian synodic years, and at the equinox eleven and one-quarter Gyrdian synodic years, following the solstice that begins the quattoural cycle, which is a winter solstice in Gyrd's northern hemisphere, Gyrd is at major perihelion, or the closest that Gyrd comes to Hysb at any point in a seven and one-half Gyrdian year period. At each minor aphelion either preceding or following the midpoint of a quattoral cycle and at each minor aphelion preceding the solstice that begins a new quattoural cycle, Gyrd is at major aphelion, or the furthest Gyrd comes to Hysb at any point in a seven and one-half Gyrdian year period. While, due to the quattoural cycle, neither minor perihelions nor minor aphelions are of uniform distance between Gyrd and Hysb, Gyrd is approximately 236,000,000 kilometers from the barycenter of Gyrd's orbit around Hysb at major perihelion and approximately 248,000,000 kilometers from the barycenter of Gyrd's orbit around Hysb at major aphelion. This puts Gyrd's orbit wholly within the outer half of Harb's circumstellar habitable zone.
As viewed from Gyrd's north geographical pole, Gyrd rotates in an anticlockwise direction. The inclination, or the orbital tilt, of Gyrd's synodic orbit relative to Hysb's equator is approximately five degrees. As Hysb appears as a disk, not a point, of light from Gyrd, and the inclination of the orbits of Hysb and Zorl relative to the invariable plane of the barycenter that Hysb and Zorl orbit are each approximately zero degrees, A total binary eclipse of Zorl by Hysb as viewed from Gyrd occurs every seven and one-half Gyrdian years.
The mean Gyrdian synodic year within any quattoral cycle is 472.2475 mean Gyrdian synodic days in length. In years in which Gyrd has a major perihelion, the Gyrdian synodic year is approximately 472.24 mean Gyrdian synodic days in length. In years in which Gyrd has a major aphelion, the Gyrdian synodic year is approximately 472.255 mean Gyrdian synodic days in length. Due to Gyrd's rotation, which is explained in more detail in the following section of this page, the Gyrdian synodic day is noticeably longer than real-life Earth's synodic day, with the mean Gyrdian synodic year measuring approximately 590.3094 Earth days in length.
Synodic rotation of Gyrd
Gyrd's synodic rotation is the rotation on its own axis relative to Hysb.
One complete rotation by Gyrd on its own axis relative to Hysb is known as a Gyrdian synodic day. The mean Gyrdian synodic day is roughly 30 Earth hours in length. There is a slight variance in the length of each Gyrdian synodic day due to Gyrd's orbit being non-circular, as well as Gyrd not having a completely consistent rotational speed. The difference between the length of Gyrd's synodic day when Gyrd is at major perihelion than the length of Gyrd's synodic day when Gyrd is at major aphelion is approximately four Earth seconds in length. The Gyrdian synodic day is at its longest when Gyrd is at major aphelion and at its shortest when Gyrd is at major perihelion.
Gyrd rotates on its own axis in an anticlockwise direction, as viewed from above Gyrd's north geographical pole. Gyrd's axial tilt, or the angle of Gyrd's axis of rotation relative to the plane of Gyrd's synodic orbit, is approximately 22.5 degrees, which is slightly less than that of real-life Earth. Gyrd's axial tilt is one of several factors contributing to Gyrd's climate patterns and meteorological seasons.
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This website does not make or imply any claim of sovereignty or control over any real-life country, nation, state, area, territory, or jurisdiction, and all content on this website is fictional unless otherwise stated.
This website does not make or imply any claim of sovereignty or control over any real-life country, nation, state, area, territory, or jurisdiction, and all content on this website is fictional unless otherwise stated.