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Daphnis (moon)

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Daphnis
Cassini probe image of Daphnis surrounded by Saturn's rings (2017)
Discovery
Discovered byCassini Imaging Science Team
Discovery dateMay 1, 2005[1]
Designations
Designation
Saturn XXXV
Pronunciation/ˈdæfnəs/[2]
Named after
Δάφνις Daphnis
S/2005 S 1
AdjectivesDaphnidian /dæfˈnɪdiən/[3]
Orbital characteristics[4]
136505.5±0.1 km
Eccentricity0.0000331±0.0000062
0.5940798 d (14.257915 h)
Inclination0.0036°±0.0013°
Satellite ofSaturn
GroupShepherd moon of the Keeler Gap
Physical characteristics
Dimensions9.8 × 8.4 × 5.6 km
(± 0.6 × 1.6 × 1.2 km)[5]: 2 
7.8±1.0 km[5]: 2 
Volume248 km3[a]
Mass(6.8±1.7)×1013 kg[5]: 3 
Mean density
0.276±0.144 g/cm3[5]: 3 
0.0002 m/s2 at longest axis
to 0.0006 m/s2 at poles
0.001 km/s at longest axis
to 0.002 km/s at poles
synchronous
unknown
Albedo≈ 0.5
Temperature≈ 78 K

Daphnis is an inner satellite of Saturn. It is also known as Saturn XXXV; its provisional designation was S/2005 S 1.[6][7] Daphnis is about 8 kilometers in diameter, and orbits the planet in the Keeler Gap within the A ring.

Naming

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The moon was named in 2006 after Daphnis, a shepherd, pipes player, and pastoral poet in Greek mythology;[8] he was descendant of the Titans, after whom the largest moons of Saturn are named. Both Daphnis and Pan, the only other known shepherd moon to orbit within Saturn's main rings, are named for mythological figures associated with shepherds.

Discovery

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Before it was photographed, the existence of a moon in Daphnis's position had already been inferred from gravitational ripples observed on the outer edge of the Keeler gap.

Daphnis was resolved into a disc for the first time in this 2005 Cassini probe image. The gravitational ripples on the edges of the rings, which had earlier hinted at the moon's presence, are clearly visible.[9]

The discovery of Daphnis was announced by the Cassini Imaging Science Team Archived 2011-05-20 at the Wayback Machine on May 6, 2005.[10] The discovery images were taken by the Cassini probe over 16 min on May 1, 2005, from a time-lapse sequence of 0.180 second narrow-angle-camera exposures of the outer edge of the A ring. The moon was subsequently found in 32 low-phase images taken of the F ring on April 13, 2005 (spanning 18 min) and again in two high-resolution (3.54 km/pixel) low-phase images taken on May 2, 2005, when its 7 km disk was resolved.

Orbit

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The inclination and eccentricity of Daphnis's orbit are very small, but distinguishable from zero. Both, particularly the inclination, are significantly greater than those of Pan (the larger moonlet which forms the Encke Gap). Daphnis's eccentricity causes its distance from Saturn to vary by ~9 km, and its inclination causes it to move up and down by ~17 km. The Keeler Gap, within which Daphnis orbits, is about 42 km wide.

Effect on Saturn's rings

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The waves that Daphnis induces nearby in the A ring have vertical relief (due to its orbital inclination) and cast shadows when Saturn is close to its equinox.

Daphnis orbits within the Keeler Gap in Saturn's dense A ring. As it orbits, it creates gravitational ripples on the edges of the gap as ring particles are attracted toward the moon and then fall back down toward the ring. The waves made by the moon in the inner edge of the gap precede it in orbit, while those on the outer edge lag behind it, due to the differences in relative orbital speed. In a photograph taken on January 18, 2017, a tendril of ring particles can be seen to extend toward the moon; according to JPL, "this may have resulted from a moment when Daphnis drew a packet of material out of the ring, and now that packet is spreading itself out."[11]

Physical characteristics

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On January 18, 2017, Daphnis was photographed from a sufficiently close distance to reveal its shape. The moon was discovered to be an irregularly-shaped object with a mostly smooth surface, a few craters, and an equatorial ridge.[11]

Notes

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  1. ^ Calculated from Daphnis's volume-equivalent sphere radius of 3.9±0.5 km given by Thomas et al. (2020)[5]: 2 

References

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  1. ^ Daphnis / IN DEPTH / BY THE NUMBERS
  2. ^ "Daphnis". Lexico UK English Dictionary. Oxford University Press. Archived from the original on March 22, 2020.
  3. ^ James Hall III (2015) Moons of the Solar System, p. 106
  4. ^ Jacobson, R. A.; Spitale, J.; et al. (2008). "Revised orbits of Saturn's small inner satellites". Astronomical Journal. 135 (1): 261–263. Bibcode:2008AJ....135..261J. CiteSeerX 10.1.1.653.3917. doi:10.1088/0004-6256/135/1/261. S2CID 122998668.
  5. ^ a b c d e Thomas, P. C.; Helfenstein, P. (July 2020). "The small inner satellites of Saturn: Shapes, structures and some implications". Icarus. 344: 20. Bibcode:2020Icar..34413355T. doi:10.1016/j.icarus.2019.06.016. S2CID 197474587. 113355.
  6. ^ C.C. Porco, et al., IAUC 8524: S/2005 S 1 May 6, 2005 (discovery)
  7. ^ Martinez, C.; and Dyches, P.; Cassini-Huygens: Cassini Finds New Saturn Moon That Makes Waves Archived 2017-05-13 at the Wayback Machine May 10, 2005
  8. ^ IAUC 8730: Saturn XXXV (Daphnis) (naming the moon)
  9. ^ NASA/JPL/Space Science Institute, "Wavemaker Moon" (2005-05-10)
  10. ^ IAUC 8524: S/2005 S 1
  11. ^ a b "Daphnis Up Close". Cassini: Mission to Saturn. Retrieved 2017-01-19.
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