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Although ERA is intended to replace sidereal time, there is a need to maintain definitions for sidereal time during the transition, and when working with older data and documents. Similarly to mean solar time, every location on Earth has its own local sidereal time (LST), depending on the longitude of the point.
The local hour angle (LHA) of an object in the observer's sky is = or = + where LHA object is the local hour angle of the object, LST is the local sidereal time, is the object's right ascension, GST is Greenwich sidereal time and is the observer's longitude (positive east from the prime meridian). [3]
Add a calculator widget to the page. Like a spreadsheet you can refer to other widgets in the same page. Template parameters Parameter Description Type Status id id The id for this input. This is used to reference it in formula of other calculator templates String required type type What type of input box Suggested values plain number text radio checkbox passthru hidden range String required ...
The equation of time is obtained by substituting the result of the right ascension calculation into an equation of time formula. Here Δ t ( M ) = M + λ p − α [ λ ( M )] is used; in part because small corrections (of the order of 1 second), that would justify using E , are not included, and in part because the goal is to obtain a simple ...
J transit is the Julian date for the local true solar transit (or solar noon). 2451545.0 is noon of the equivalent Julian year reference. 0.0053 sin M − 0.0069 sin ( 2 λ ) {\displaystyle 0.0053\sin M-0.0069\sin \left(2\lambda \right)} is a simplified version of the equation of time .
As seen from above the Earth's north pole, a star's local hour angle (LHA) for an observer near New York. Also depicted are the star's right ascension and Greenwich hour angle (GHA), the local mean sidereal time (LMST) and Greenwich mean sidereal time (GMST). The symbol ♈︎ identifies the March equinox direction.
Local mean time (LMT) is a form of solar time that corrects the variations of local apparent time, forming a uniform time scale at a specific longitude. This measurement of time was used for everyday use during the 19th century before time zones were introduced beginning in the late 19th century; it still has some uses in astronomy and navigation.
For the evaluation of the images, a special Excel spreadsheet has been developed. For three stars, the rectangular X-Y-coordinates are measured at both ends of their trails or on both static images. In addition, we need the current right ascension and declination of the 3 stars, the longitude and latitude of the observatory, and the date and ...