PROBA-3

Proba-3

An artistic rendering of PROBA-3.
Mission type	Solar observatory technology demonstrator
Operator	ESA
Website	link
Mission duration	2 years (nominal)
Spacecraft properties
Manufacturer	S/C: SENER/Redwire/EADS CASA/GMV/SPACEBEL ASPIICS: CSL
Launch mass	CSC and OSC in stack: 550 kilograms (1,210 lb)
Dimensions	CSC: 1.1 by 1.8 by 1.7 metres (3.6 ft × 5.9 ft × 5.6 ft) OSC: 0.9 by 1.4 metres (3.0 ft × 4.6 ft)
Start of mission
Launch date	5 December 2024 (planned)[1]
Rocket	PSLV-XL C-59 [2]
Launch site	First Launch Pad,Satish Dhawan Space Centre
Contractor	NSIL ISRO
Orbital parameters
Reference system	Geocentric
Regime	Highly-elliptical Earth Orbit
Semi-major axis	36,943 kilometres (22,955 mi)
Eccentricity	0.8111
Perigee altitude	600 kilometres (370 mi)
Apogee altitude	60,530 kilometres (37,610 mi)
Inclination	59 degrees
Period	19.7 hours
RAAN	153 degrees
Argument of perigee	188 degrees
Epoch	planned
PROBA-series ← PROBA-V

Proba-3 is a dual probe technological demonstration mission by the European Space Agency devoted to high precision formation flying to achieve scientific coronagraphy. It is part of the series of PROBA satellites that are being used to validate new spacecraft technologies and concepts while also carrying scientific instruments.

The mission concept dates back to 2005 when a study was performed in the ESA CDF. After several phase A studies and a change of industrial organisation at the beginning of the phase B,^[3] the mission's implementation phase (Phases C/D/E1) eventually began in July 2014.^[4]

The system Critical Design Review was completed in 2018.^[5]

The two spacecraft integration before environmental campaign was completed as of March 2023.^[6]

The project is managed by Damian Galano.^[7]

Proba-3 consists of two independent, three-axis stabilized spacecraft: the Coronagraph Spacecraft (CSC) and the Occulter Spacecraft (OSC). Both spacecraft will fly close to each other on a highly elliptical orbit around the Earth, with an apogee at 60,500 km altitude.^[4][8][9]

ESA said that by flying in tight formation about 150 metres apart, the Occulter will precisely cast its shadow onto the Coronagraph’s telescope, blocking the Sun’s direct light. This will allow the Coronagraph to image the faint solar corona in visible, ultraviolet and polarised light for many hours at a time.^[10]

Along the apogee arc, when the gravity gradient is significantly smaller, the two spacecraft will autonomously acquire a formation configuration, such that the CSC remains at a fixed position in the shadow cast by the OSC. The CSC hosts a coronagraph which will then be able to observe the Sun's Corona without being blinded by the intense light from the photosphere. Given the diameter of the occulter disk on the OSC and the intended Corona observation regions, the CSC must be approximately 150 meters from the OSC, and maintain this position with millimetric accuracy, both in range and laterally. The scientific objective is to observe the Corona down to about 1.1 solar radius in the visible wavelength range.

Besides formation flying for coronagraphy, some formation flying demonstration manoeuvers (retargeting and resizing manoeuvers) will be attempted during the apogee phase of the orbit, as well as a space rendezvous experiment.^[9]

The formation acquisition and control is performed on-board thanks to a set of metrology equipment and actuators. The metrology equipment comprise a laser based system providing high accuracy relative position estimate, a visual based sensor with a coarser precision but wider field of view, and a shadow position sensor providing finest precision when the CSC is in the vicinity of the target position in the shadow cone.

After the apogee arc, the formation is broken by impulsive manoeuvers executed by the spacecraft. The two spacecraft are placed on a relative trajectory that passively ensures no risk of collision during the perigee passage, when the spacecraft altitude goes down to 600 km. Along the perigee phase of the orbit, the two spacecraft acquire GNSS data to derive a precise estimation of the relative position and velocity that is propagated for a few hours up to the reacquisition of the metrology before the next apogee arc.

The CSC and OSC exchange sensor data and commands through a RF (radio frequency) based inter-satellite link to coordinate their activities.Scientists hope Proba-3’s unique vantage point will provide new insights into the origins of coronal mass ejections (CMEs) — eruptions of solar material that can disrupt satellites and power grids on Earth. The mission will also measure total solar irradiance, tracking changes in the Sun’s energy output that may influence Earth’s climate.^[10]

The CSC is a 300 kg mini-satellite, hosting the coronagraph ASPIICS and the shadow position sensors. It is equipped with a mono-propellant propulsion system to perform the large delta-V manoeuver necessary for formation acquisition and breaking. It also hosts the targets used by the metrology optical heads on board the OSC.

The OSC is a 250 kg mini-satellite, hosting the laser and visual metrology optical heads. It features the occulter disk that is 1.4 meter in diameter. The shape of its rim is intended to reduce the amount of sun diffracted light entering the coronagraph. The OSC uses a low-thrust cold gas propulsion system that enables the fine position control required for the formation flying.

The primary payload is the ASPIICS Coronagraph. Its follows the design concept of a classical externally occulted Lyot coronagraph, with the external occulter physically attached to the OSC while the rest of the instrument is on the CSC.^[11]

ASPIICS will observe the solar corona through refractive optics, able to select 3 different spectral bands: Fe XIV line @ 530.4 nm, He I D3 line @587.7 nm, and the white-light spectral band [540;570 nm].^[12]

It is expected that the data from ASPIICS will fill the gap in term of field of view between EUV imagers and externally occulted coronagraphs, when the latter are monolithic instruments that don't benefit from the longer distance enabled by formation flying.^[13]

The Principal Investigator for the coronagraph instrument is Andrei Zhukov from Royal Observatory of Belgium.^[14][7]

A secondary scientific payload (DARA) is hosted on the OSC. DARA stands for Davos Absolute Radiometer and is an absolute radiometer for measuring Total Solar Irradiance (TSI).^[15]

Like the other Proba satellites, PROBA-3 will be operated from the ESA center in Redu, Belgium.^[16]

Proba-3 is a project managed by the European Space Agency. The industrial development of the S/C and the ground segment is led by SENER Aerospace^[17][18] which coordinates the work of a core team with Airbus Defence and Space, Qinetiq Space, GMV, Celestia Antwerp BV and Spacebel.

The Coronagraph payload is developed for ESA by a consortium led by Liège Space Center (CSL) in Belgium, made up of 15 companies and institutes from five ESA Member States.^[18]

DARA is provided by the PMOD institute in Switzerland.^[13]

Testing of the mission's vision-based sensor system was performed at ESA's ESTEC technical centre in the Netherlands in March 2021. The system will enable the two spacecraft to fly in a precise formation. The testing reportedly yielded promising results.^[19].The miniature satellites recently underwent final integration and were viewed in person by Proba-3’s Science Working Team. Members of the team plan to test flight hardware during April's total solar eclipse over North America, gaining valuable experience for interpreting Proba-3’s future results^[10]

• Prisma
• ESA's PROBA missions:
  • PROBA-1
  • PROBA-2
  • PROBA-V

• Official website
• eoPortal PROBA-3 page