fn ecliptic_cartesian_coords(&self, day: f64) -> Array3d {
        let d = day - 1.5;
        // Julian centuries since J2000.0
        let t = d / 36525.0;
        // Sun's mean longitude, in degrees
        let l_0 = 280.46645 + (36000.76983 * t) + (0.0003032 * t * t);
        // Sun's mean anomaly, in degrees
        let m_0 = 357.52910 + (35999.05030 * t) - (0.0001559 * t * t) - (0.00000048 * t * t * t);

        let c = // Sun's equation of center in degrees
            (1.914600 - 0.004817 * t - 0.000014 * t * t) * sin_deg!(m_0) +
                (0.01993 - 0.000101 * t) * sin_deg!(2f64 * m_0) +
                0.000290 * sin_deg!(3f64 * m_0);

        let ls = l_0 + c; // true elliptical longitude of Sun

        // The eccentricity of the Earth's orbit.
        let e = 0.016708617 - t * (0.000042037 + (0.0000001236 * t));
        // distance from Sun to Earth in astronomical units (AU)
        let distance_in_au = (1.000001018 * (1f64 - e * e)) / (1f64 + e * cos_deg!(m_0 + c));
        let mut x = -distance_in_au * cos_deg!(ls);
        let mut y = -distance_in_au * sin_deg!(ls);

        // Convert AU to Meters
        x *= AU_METER;
        y *= AU_METER;

        // the Earth's center is always on the plane of the ecliptic (z=0), by definition!
        Array3d { x, y, z: 0f64 }
    }
/// Calculate the position of Earth relative to the Sun.
/// Calls function earth_ecliptic_cartesian_coords in kepler_utilities
///
///  ### Arguments
/// * 'day' - Day as an f64
///
/// ### Return
///     The coordinates of Earth at the provided time.
Calculate the position of Earth relative to the Sun.

Arguments
'day' - Day as an f64
Calculate the position of Earth relative to the Sun . Arguments ' day ' - Day as an f64
fn ecliptic_cartesian_coords(&self, day: f64) -> Array3d {
        let d = day - 1.5;
        // Julian centuries since J2000.0
        let t = d / 36525.0;
        // Sun's mean longitude, in degrees
        let l_0 = 280.46645 + (36000.76983 * t) + (0.0003032 * t * t);
        // Sun's mean anomaly, in degrees
        let m_0 = 357.52910 + (35999.05030 * t) - (0.0001559 * t * t) - (0.00000048 * t * t * t);
        let c = // Sun's equation of center in degrees
            (1.914600 - 0.004817 * t - 0.000014 * t * t) * sin_deg!(m_0) +
                (0.01993 - 0.000101 * t) * sin_deg!(2f64 * m_0) +
                0.000290 * sin_deg!(3f64 * m_0);
        let ls = l_0 + c; // true elliptical longitude of Sun
        // The eccentricity of the Earth's orbit.
        let e = 0.016708617 - t * (0.000042037 + (0.0000001236 * t));
        // distance from Sun to Earth in astronomical units (AU)
        let distance_in_au = (1.000001018 * (1f64 - e * e)) / (1f64 + e * cos_deg!(m_0 + c));
        let mut x = -distance_in_au * cos_deg!(ls);
        let mut y = -distance_in_au * sin_deg!(ls);
        // Convert AU to Meters
        x *= AU_METER;
        y *= AU_METER;
        // the Earth's center is always on the plane of the ecliptic (z=0), by definition!
        Array3d { x, y, z: 0f64 }
    }
fn ecliptic_cartesian_coords ( & self , day : f64 ) -> Array3d { let d = day - 1.5 ; // Julian centuries since J2000.0 let t = d / 36525.0 ; // Sun's mean longitude, in degrees let l_0 = 280.46645 + ( 36000.76983 * t ) + ( 0.0003032 * t * t ) ; // Sun's mean anomaly, in degrees let m_0 = 357.52910 + ( 35999.05030 * t ) - ( 0.0001559 * t * t ) - ( 0.00000048 * t * t * t ) ; let c = // Sun's equation of center in degrees ( 1.914600 - 0.004817 * t - 0.000014 * t * t ) * sin_deg ! ( m_0 ) + ( 0.01993 - 0.000101 * t ) * sin_deg ! ( 2f64 m_0 ) + 0.000290 * sin_deg ! ( 3f64 m_0 ) ; let ls = l_0 + c ; // true elliptical longitude of Sun // The eccentricity of the Earth's orbit. let e = 0.016708617 - t * ( 0.000042037 + ( 0.0000001236 * t ) ) ; // distance from Sun to Earth in astronomical units (AU) let distance_in_au = ( 1.000001018 * ( 1f64 - e * e ) ) / ( 1f64 + e * cos_deg ! ( m_0 c ) ) ; let mut x = - distance_in_au * cos_deg ! ( ls ) ; let mut y = - distance_in_au * sin_deg ! ( ls ) ; // Convert AU to Meters x *= AU_METER ; y *= AU_METER ; // the Earth's center is always on the plane of the ecliptic (z=0), by definition! Array3d { x , y , z : 0f64 } }
Calculate the position of Earth relative to the Sun.
Calculate the position of Earth relative to the Sun .
The coordinates of Earth at the provided time.
The coordinates of Earth at the provided time .
&self
day
f64