Calculation of radial velocity, introduction of radial velocity

I just checked the calculation, and the question is indeed wrong, so it should be correct.

First of all, we need to understand that the radial velocity of a star relative to the heliocentric center is broken down into two parts, one is the radial velocity that we observe on Earth, and the other is the projection of the Earth's relative solar velocity in the direction of line of sight. The first velocity, which can be easily calculated by multiplying the blueshift by the speed of light, is that the minus sign indicates that it is facing us.

The next step, and the most difficult, is to calculate how the Earth's velocity is projected in the direction of the line of sight. The speed of the earth's revolution is, when the sun's ecliptic longitude is 100 degrees, assuming that the direction of the earth's motion is perpendicular to this direction, then the direction of the earth's movement is 10 degrees of ecliptic longitude. For the convenience of calculation, we also convert the stellar coordinates to the ecliptic coordinate system, which can be used by **calculators.

I use this to calculate, and get the result yellow longitude, yellow latitude, since I have the spherical coordinates of the earth's velocity and the direction of the line of sight, I can get the cosine of the angle between these two directions, since you are studying mathematics, I don't need to teach you, the cosine value is calculated, and the speed multiplied is. This number is added to the previous velocity, so it is.

I'm an astrophysics student, and there's a lot of stuff in it that is hard for a layman to understand, and I don't know why you're doing that.

The right ascension and declination of so many celestial bodies, and the ecliptic longitude of the sun, were actually given to eliminate the Doppler effect caused by the rotation of the Earth.

After deducting the change in radial velocity caused by the earth, we can get the radial velocity relative to the sun. First, convert the right ascension and declination into yellow longitude and yellow latitude (spherical triangles will not, only check the software), and then calculate the projection of the speed of the Earth's motion on the line between the Earth and the star. In this way, an astronomical problem is transformed into a process that is not too complicated in mathematics and physics.

I doubt the answer, the approaching blue shift, the speed of the radial movement is only a few tens of kilometers per second? Is the observed wavelength wrong by one bit, should it be "?

I can only give some of the above ideas for the landlord's question, as for the detailed mathematical calculations, the mathematical skills are too poor, and there is really nothing that can be done. The landlord's problem is quite professional, knowing that this popular science platform may not be able to solve such a complex problem, please go to the relevant astronomy (it seems to be rare) and physics forums for help.

Ray velocity is the velocity of an object towards the direction of the line of sight. An object's rays will be governed by the Doppler effect in terms of radial velocity, with the wavelength of the degraded object increasing (redshifted) and approaching objects decreasing (blueshifted).

Ray velocity is the velocity of an object towards the direction of the line of sight. The radial velocity of an object's light will be matched by the Doppler effect, and the wavelength of the degraded object will increase (redshift), while the wavelength of the approaching object will decrease (blueshirt). The radial velocity of a star can be accurately measured by high-resolution spectra and compared to known spectral line wavelengths measured in the laboratory.

Traditionally, a positive radial velocity indicates that the object is receding, and if it is negative, the object is approaching.

In many binions, orbital motion usually results in a change in radial velocity of several kilometers per second. It is suspected that the variation of the spectral lines of these stars is due to the Doppler effect, so they are called spectral glopheries. Studying radial velocity can estimate the mass of a star and some orbital elements, such as eccentricity and semi-major axis.

The same method is used to discover planets orbiting stars, where the measured motion can determine the orbital period of the planet, and the magnitude of the displacement can be used to calculate the mass of the planet.