The procedure for calculating the heliocentric polar coordinates (r,θ) of a planet as a function of the time t since perihelion, is the following five steps: Compute the mean motion n = (2π rad)/P, where P is the period. Compute the mean anomaly M = nt, where t is the time since perihelion. Compute the eccentric anomaly E by solving Kepler'sAt our sun’s distance from the center of the Milky Way, it’s rotating once about every 225-250 million years – defined by the length of time the sun takes to orbit the center of the galaxy. The method is quite simple. Take one photo shortly after sunset using a small aperture like f/11 to get substantial depth of field. Then, keep your tripod in the same spot until the Milky Way rises. Take a second photo at your usual astrophotography settings – say, f/1.8 and focused on the stars.
Step 1/4 1. The Milky Way takes about 225-250 million years to complete one rotation. Step 2/4 2. If we assume the Milky Way formed 13.5 billion years ago, we can calculate the number of rotations by dividing the age of the galaxy by the time it takes to complete one rotation: 13,500,000,000 years / 250,000,000 years = 54 rotations (approximately).
Back in the 2020s we had never seen the Milky Way from the outside, but it was known to be a vast spiral about 100,000 light years across, with a central bar of densely packed stars.
The James Webb Space Telescope captured the Cartwheel galaxy, which is around 500 million light-years away, in a photo released by NASA on August 2. NASA/ESA/CSA/STScI. Webb's landscape-like viewThere have been many particularly exhilarating eras in the past 175 years—the 1920s and 1930s, when we realized the universe was not limited to the Milky Way, and the 1960s and 1970s, when we W8cIGe9.