Heliocentric Julian Day

The correction is zero (HJD = JD) for objects at the poles of the ecliptic. Elsewhere, it is approximately an annual sine curve, and the highest amplitude occurs on the ecliptic. The maximum correction corresponds to the time in which light travels the distance from the Sun to the Earth, i.e. ±8.3 min (500 s, 0.0058 days).

JD and HJD are defined independent of the time standard. Rather, JD can be expressed as e.g. UTC, UT1, TT or TAI. The differences between these time standards are of the order of a minute, so that for minute accuracy of timings the standard used has to be stated. The HJD correction involves the heliocentric position of the Earth, which is expressed in TT. While the practical choice may be UTC, the natural choice is TT.

Since the Sun itself orbits around the barycentre of the Solar System, the HJD correction is not actually to a fixed reference. The difference between correction to the heliocentre and to the barycentre is up to ±4 s. For second accuracy, the Barycentric Julian Date (BJD) should be calculated instead of the HJD.

The common formulation of the HJD correction assumes that the object is at infinite distance, certainly beyond the Solar System. The resulting error for Edgeworth-Kuiper Belt objects would be 5 s, and for objects in the main asteroid belt it would be 100 s. In this calculation, the Moon – which is closer than the Sun – can be wrongly placed on the far side of the Sun, resulting in an error of about 15 min.

In terms of the vector ${\displaystyle {\vec {r}}}$ from the heliocentre to the observer, the unit vector ${\displaystyle {\hat {n}}}$ from the observer toward the object or event, and the speed of light ${\displaystyle c}$:

$${\displaystyle HJD=JD+{\frac {{\vec {r}}\cdot {\hat {n}}}{c}}}$$

When the scalar product is expressed in terms of the right ascension ${\displaystyle \alpha }$ and declination ${\displaystyle \delta }$ of the Sun (index ${\displaystyle \odot }$) and of the extrasolar object this becomes:

$${\displaystyle HJD=JD-{\frac {r}{c}}\cdot [\sin(\delta )\cdot \sin(\delta _{\odot })+\cos(\delta )\cdot \cos(\delta _{\odot })\cdot \cos(\alpha -\alpha _{\odot })]}$$

where ${\displaystyle r}$ is the distance between Sun and observer. The same equation can be used with any astronomical coordinate system. In ecliptic coordinates the Sun is at latitude zero, so that

$${\displaystyle HJD=JD-{\frac {r}{c}}\cdot \cos(\beta )\cdot \cos(\lambda -\lambda _{\odot })}$$

• Barycentric Julian Date
• Time standard

• Eastman, Jason; Siverd, Robert; Gaudi, B. Scott (2010). "Achieving Better Than 1 Minute Accuracy in the Heliocentric and Barycentric Julian Dates". Publications of the Astronomical Society of the Pacific. 122 (894): 935–946. arXiv:1005.4415. Bibcode:2010PASP..122..935E. doi:10.1086/655938. S2CID 54726821.
• A. Hirshfeld, R.W. Sinnott (1997). Sky catalogue 2000.0, volume 2, double stars, variable stars and nonstellar objects, p. xvii. Sky Publishing Corporation (ISBN 0-933346-38-7) and Cambridge University Press (ISBN 0-521-27721-3).

• http://astroutils.astronomy.ohio-state.edu/time/: Online converter from UTC to BJD_TDB, BJD_TDB to UTC, or HJD (UTC or TT) to BJD_TDB.