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// Workers AI · dad joke modeWhat did C/2004 Q2 (Machholz) say? Comet me maybe?

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(Redirected from C/2004 Q2)

C/2004 Q2 (Machholz)
Comet Machholz photographed by Ralf Weber from Andalusia, Spain in February 2005
Discovery
Discovered byDonald E. Machholz
Discovery date27 August 2004
Orbital characteristics[1][2]
Epoch30 March 2005 (JD 2453459.52005)
Observation arc2.03 years
Number of
observations		3,612
Aphelion~5,100 AU (inbound)
~1,100 AU (outbound)
Perihelion1.205 AU
Semi-major axis~2,400 AU
Eccentricity0.99950
Orbital period~130,000 years (inbound)
~12,400 years (outbound)
Inclination38.589°
93.622°
Argument of
periapsis		19.505°
Mean anomaly0.001°
Last perihelion24 January 2005
TJupiter1.066
Earth MOID0.249 AU
Jupiter MOID1.973 AU
Physical characteristics[2]
Dimensions4.2–7.8 km (2.6–4.8 mi)[3]
Mean diameter
6.0 km (3.7 mi)[3]
Mass1.0×1013 kg[4]
Mean density
450±70 kg/m3[5]
9.1±0.2 hours[6]
Comet total
magnitude (M1)		11.2

Comet Machholz, formally designated as C/2004 Q2, is a non-periodic comet discovered by Donald Machholz on 27 August 2004. It reached naked eye brightness in January 2005. Unusual for such a relatively bright comet, its perihelion was farther from the Sun than the Earth's orbit.

Physical characteristics

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During its closest approach to Earth in January 2005, ground observations from La Palma, Spain revealed that the comet may have a rotation period of 9.1±0.2 hours,[6] although a 2012 study regarding the morphological structures in its coma suggested it may have a rotation period of 0.74 days instead.[7]

Between December 2004 and January 2005, observations from Lulin and La Silla observatories spotted two jets of carbon and cyanogen (CN) compounds that form a spiral-like structure within the coma, which were caused by two active surface regions in its nucleus.[8] In March 2005, the GALEX spacecraft observed the comet in far-ultraviolet (FUV) light, where it determined that ionized methane (CH4) molecules dominated its coma, which explained the shorter than expected lifetime of carbon molecules detected.[9] Spectral analysis of this comet's chemical composition suggest that it may have formed in a relatively inner region of the solar nebula than other typical Oort cloud comets, at a distance of at least 5.0 AU (750 million km) from the Sun.[10] Additionally, the methane molecules frozen in the comet and its ratio relative to water indicate formation at relatively high temperatures compared to other comets.[11]

Near-infrared measurements of the comet has indicated that its surface material generate an outflow in the form of fragments that separated into gas and dust under sublimation on time scales of the order of days.[12]

Its nucleus has a mean diameter of 6.0 km (3.7 mi).[3]

Orbit

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C/2004 Q2 appears to pass near the Pleiades cluster in 2005.

Given the orbital eccentricity of this object, different epochs can generate quite different heliocentric unperturbed two-body best-fit solutions to the aphelion distance (maximum distance) of this object. For objects at such high eccentricity, the Suns barycentric coordinates are more stable than heliocentric coordinates. Using JPL Horizons the barycentric orbital elements for epoch 2050 generate a semi-major axis of 537 AU (80.3 billion km) and a period of approximately 12,400 years.[1]

See also

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References

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  1. 1 2 Horizons output. "Barycentric Osculating Orbital Elements for Comet C/2004 Q2 (Machholz)". Solution using the Solar System Barycenter. Ephemeris Type:Elements and Center:@0 (To be outside planetary region, inbound epoch 1950 and outbound epoch 2050)
  2. 1 2 "C/2004 Q2 (Machholz) – JPL Small-Body Database Lookup". ssd.jpl.nasa.gov. Jet Propulsion Laboratory. Retrieved 31 May 2025.
  3. 1 2 3 D. C. Jewitt (2022). "Destruction of Long-period Comets". The Astronomical Journal. 164 (4): 158–166. arXiv:2208.04469. Bibcode:2022AJ....164..158J. doi:10.3847/1538-3881/ac886d.
  4. ↑ A. Sosa; J. A. Fernández (2011). "Masses of long-period comets derived from non-gravitational effects" (PDF). Monthly Notices of the Royal Astronomical Society. 416 (1): 767–782. doi:10.1111/j.1365-2966.2011.19111.x.
  5. ↑ M. L. Paradowski (2022). "A New Indirect Method of Determining Density of Cometary Nuclei" (PDF). Acta Astronomica. 72 (2): 141–159. Bibcode:2022AcA....72..141P. doi:10.32023/0001-5237/72.2.4. ISSN 0001-5237.
  6. 1 2 M. Reyniers; P. Degroote; D. Bodewits; J. Cuypers; C. Waelkens (2009). "The rotation and coma profiles of comet C/2004 Q2 (Machholz)" (PDF). Astronomy & Astrophysics. 494 (1): 379–389. arXiv:0812.2398. doi:10.1051/0004-6361:20079225.
  7. ↑ F. Manzini; R. Behrend; L. Comolli; V. Oldani; C. B. Cosmovici; et al. (2012). "Comet Machholz (C/2004 Q2): morphological structures in the inner coma and rotation parameters". Astrophysics and Space Science. 337 (2). arXiv:1109.4163. Bibcode:2012Ap&SS.337..531M. doi:10.1007/s10509-011-0866-8.
  8. ↑ Z. Y. Lin; M. Weiler; H. Rauer; W. H. Ip (2007). "Photometry and imaging of comet C/2004 Q2 (Machholz) at Lulin and La Silla". Astronomy & Astrophysics. 469 (2): 771–776. Bibcode:2007A&A...469..771L. doi:10.1051/0004-6361:20077286.
  9. ↑ J. P. Morgenthaler; W. M. Harris; M. R. Combi; P. D. Feldman; H. A. Weaver (2010). "GALEX FUV Observations of Comet C/2004 Q2 (Machholz): The Ionization Lifetime of Carbon". The Astrophysical Journal. 426 (1): 1–10. arXiv:1011.4313. Bibcode:2011ApJ...726....8M. doi:10.1088/0004-637X/726/1/8.
  10. ↑ H. Kobayashi; H. Kawakita (2009). "Formation Conditions of Icy Materials in Comet C/2004 q2 (Machholz). I. Mixing Ratios of Organic Volatiles" (PDF). The Astrophysical Journal. 703 (1): 121–130. Bibcode:2009ApJ...703..121K. doi:10.1088/0004-637X/703/1/121.
  11. ↑ H. Kobayashi; H. Kawakita (2009). "Formation Conditions of Icy Materials in Comet C/2004 Q2 (Machholz). II. Diagnostics Using Nuclear Spin Temperatures and Deuterium-to-Hydrogen Ratios in Cometary Molecules". The Astrophysical Journal. 693 (1): 388–396. Bibcode:2009ApJ...693..388K. doi:10.1088/0004-637X/693/1/388.
  12. ↑ I. A. Maslov; A. E. Nadzhip; V. I. Shenavrin (2008). "Near-infrared observations of Comet C/2004 Q2 (Machholz)". Astronomy Letters. 34 (5): 353–356. Bibcode:2008AstL...34..353M. doi:10.1134/S1063773708050083.
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