Outer Moons of Jupiter

My DLR colleague Stefano Mottola and I perform an observation campaign of the irregular satellites of Jupiter to measure lightcurves for rotation period, spin-axis orientation, and shape determination. For this task, we use the 1.23-m telescope at Calar Alto in southern Spain which allows us to observe the largest of Jupiter’s outer moons in greater detail. Mein DLR Kollege Stefano Mottola und ich führen eine Beobachtungskampagne der irregulären Jupitermonde durch, um Lichtkurven zur Bestimmung der Rotationsperioden, Polachsenausrichtungen sowie der Formen der Objekte zu erhalten. Für diese Aufgabe verwenden wir das 1.23-m Teleskop auf dem Calar Alto in Südspanien, mit dem wir die größten der irregulären Jupitermonde im Detail studieren können.

Paper on Himalia’s rotation period: Pilcher, F., Mottola, S., Denk, T. (2012): Photometric Lightcurve and Rotation Period of Himalia (Jupiter VI). Icarus 219, 741-742. doi:10.1016/j.icarus.2012.03.021.

Paper on Cassini’s Jupiter flyby in Dec 2000, including observations of Himalia: Porco, C.C., 23 colleagues (2003): Cassini Imaging of Jupiter’s Atmosphere, Satellites, and Rings. Science 299, no. 5612, 1541-1547. doi:10.1126/science.1079462.
Another source for this paper is here. An excerpt of the part describing the Himalia findings can be found here.

Calar-Alto related webpages:
Weather forecast (continuous live data stream)
Current Meteosat weather picture
Calar-Alto webcams (continuous live data stream); the WEST and NORTH views show the 1.23-m telescope

Planning-related webpage:
HORIZONS Web-Interface

Table: Physical and astronomical properties of the largest irregular moons of Jupiter

Moon Spice ID1 Orbit2 Apparent magnitude
Absolute magnitude
H [mag]4
Visible albedo range
Mean diameter
Rotation period
Semi-major axis
[million km]7
[ ]7
Orbital period
Moon (abbrev.)8
Themisto 518 prograde 21.0 14.4 4 ? ∼9 ? 7.40 0.24 46 132.0 The
Himalia 506 prograde 14.8 8.0 4.9–6.5 120×150 7.7819 11.46 0.15 30 254.3 Him
Elara 507 prograde 16.6 9.5 3.9–5.3 80 ? 11.70 0.17 30 262.5 Ela
Lysithea 510 prograde 18.2 11.1 3.0–4.2 42 (12.8) 11.67 0.12 27 261.4 Lys
Leda 513 prograde 20.2 12.6 2.8–4.0 22 ? 11.17 0.16 28 244.8 Led
Pasiphae 508 retrograde 16.9 10.2 3.8–5.0 58 ? 23.08 0.60 153 726.8 Pas
Carme 511 retrograde 17.9 10.9 2.9–4.1 47 (10.4) 22.49 0.34 166 699.2 Car
Sinope 509 retrograde 18.3 11.3 3.6–4.8 35 (13.2) 23.67 0.30 159 754.8 Sin
Ananke 512 retrograde 18.9 11.8 3.2–4.4 29 (8.3) 20.84 0.24 148 623.8 Ana
Callirrhoe 517 retrograde 20.8 13.9 3.6–6.8 10 ? 23.21 0.52 148 733.1 Cal
Praxidike 527 retrograde 21.2 15.2 2.3–3.5 7 ? 20.72 0.33 147 618.1 Pra

Table notes:

1…SPICE is a commonly-used information system of NASA’s Navigation and Ancillary Information Facility (NAIF). It assists engineers in modeling, planning, and executing planetary-exploration missions, and supports observation interpretation for scientists. Each planet and moon obtained a unique SPICE number.

2…The irregular satellites of Jupiter can be subdivided into objects with prograde and objects with retrograde orbits. Themisto is the irregular moon closest to the planet. The moons in the prograde Himalia group share an inclination close to 28°. The retrograde irregulars orbit Jupiter in three distinct groups at inclinations ranging from 144° to 165°. The naming convention is that all prograde irregular moons of the Himalia group have names ending with an ‘a’, the other prograde irregulars have names ending with ‘o’, and the retrograde moons’s names end with an ‘e’. As of end-of-January 2018, 7 prograde and 54 retrograde irregular Jovian moons were known. About a dozen of the retrogrades were in danger of getting lost (Jacobson et al. 2012; see also JPL’s SSD websites), but it appears that a successful recovery of all of them was possible in 2017.

3Apparent magnitude as seen from Earth (R-band); from S. Sheppard’s Jupiter satellites website. Smaller numbers indicate brighter objects. The magnitude scale is logarithmic, with an object of 6th mag being 100x darker than a 1st mag object. The human eye can spot celestial objects down to ∼6th magnitude.

4…The absolute magnitude is the magnitude (brightness) of an object if located 1 au away from the sun and observed at 0° phase angle (i.e., the observer virtually sits at the center of the sun in this definition). Smaller numbers again indicate brighter objects. The values listed here were taken from Table 1 of the paper of Grav et al. (2015) who refers to Rettig et al. (2001). The Themisto value is from S. Sheppard’s page. Be aware that different sources list quite different values for H; e.g., compare with values from MPECa NASA Fact Sheet, JPL’s ssd page, S. Sheppard, or Table 12.1 in Jewitt et al. (2004) (which has the same values as the Sheppard site).

5…Albedos and diameters are from WISE and NEOWISE data published in Table 3 of Grav et al. (2015). The axes of Himalia are from our Cassini work, published in Porco et al. (2003). The Themisto diameter is again from S. Sheppard; the Themisto albedo is a guess.

6…All values are synodic rotation periods. The Himalia value is from our Pilcher et al. (2012) paper. The Lysithea, Sinope, Carme, and Ananke periods are from Luu (1991). Because of the short observation timelines, they are likely inaccurate and thus notated in brackets only. Luu (1991) also observed Elara, Pasiphae, and Leda, but could not deduce periods.
For Elara, Wikipedia gives ∼0.5 d. JPL’s HORIZONS Web-Interface also has this value, but I could not find a proper source from where they got it. Maybe it was taken from Table 6.1 in Stanton Peale’s chapter in the 1977 Planetary Satellites book of the University of Arizona Press? If so, it would definitely be wrong because all unknown periods in this table are listed as “0.5 d”. Thus, no Elara rotation period is added to my table here.
Leda was observed by Rettig et al. (2001) over three consecutive nights, but they could not extract a rotation period. They thus note ∼24 h as a possible value for Leda, but I do not believe that. (A non-detection of a period does not necessarily point to a period close to Earth’s. It may also mean that the equatorial cross-section of the object is rather spherical with no prominent albedo markings, that the object’s pole axis was pointing close to the observer, that the rotation itself is very slow, or that the observation’s signal-to-noise ratio was insufficient.)

7…The data for the orbital parameters were taken from MPEC (January 2018). For the orbit period, I used the values of the orbit frequency n and converted them into units of days.

8…These abbreviations are my own and not official.

© Tilmann Denk (2018)