Asteroid 11 Parthenope will be well placed for observation, lying in the constellation Aquarius, well above the horizon for much of the night.
Regardless of your location on the Earth, 11 Parthenope will reach its highest point in the sky around midnight local time.
From Cambridge, it will be visible between 21:59 and 03:37. It will become accessible around 21:59, when it rises to an altitude of 21° above your south-eastern horizon. It will reach its highest point in the sky at 00:50, 33° above your southern horizon. It will become inaccessible around 03:37 when it sinks below 22° above your south-western horizon.
The geometry of the alignment
This optimal positioning occurs when it makes its closest approach to the point in the sky directly opposite to the Sun – an event termed opposition. Since the Sun reaches its greatest distance below the horizon at midnight, the point opposite to it is highest in the sky at the same time.
At around the same time that 11 Parthenope passes opposition, it also makes its closest approach to the Earth – termed its perigee – making it appear at its brightest in the night sky. This happens because when 11 Parthenope lies opposite to the Sun in the night sky, the solar system is lined up so that 11 Parthenope, the Earth and the Sun lie in a straight line with the Earth in the middle, on the same side of the Sun as 11 Parthenope.
On this occasion, 11 Parthenope will pass within 1.203 AU of us, reaching a peak brightness of magnitude 8.8. Nonetheless, even at its brightest, 11 Parthenope is a faint object beyond the reach of the naked eye; binoculars or a telescope of moderate aperture are needed.
Finding 11 Parthenope
The chart below indicates the path of 11 Parthenope across the sky around the time of opposition.
The position of 11 Parthenope at the moment of opposition will be as follows:
|Asteroid 11 Parthenope||22h28m40s||-13°47'||Aquarius||8.8|
The coordinates above are given in J2000.0.
|The sky on 06 April 2020|
13 days old
All times shown in EDT.
The circumstances of this event were computed from orbital elements made available by Ted Bowell of the Lowell Observatory. The conversion to geocentric coordinates was performed using the position of the Earth recorded in the DE405 ephemeris published by the Jet Propulsion Laboratory (JPL).
The star chart above shows the positions and magnitudes of stars as they appear in the Tycho catalogue. The data was reduced by the author and plotted using PyXPlot. A gnomonic projection of the sky has been used; celestial coordinates are indicated in the J2000.0 coordinate system.