The Nucleus of Comet Hyakutake (C/1996 B2)

Lisse, C. M.; Fernández, Y. R.; Kundu, Arunav; A’Hearn, Michael F.; Dayal, Aditya; Deutsch, L. K.; Fazio, G. G.; Hora, J. L.; Hoffmann, W. F.

doi:10.1006/icar.1999.6131

Cited by 74 publications

(73 citation statements)

References 38 publications

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“…Fig. 5 shows the value of P critical period in h for values of a/b allowable by our results and ρ for different Solar System asteroid taxonomic types from comets, Dtypes with 0.5-1.0 g cm −3 , B and C-types with 1.2-1.4 g cm −3 , S-types with 2.3 g cm −3 , X-types with 2.7 g cm −3 , rubble piles with 3.3 g cm −3 and 4 g cm −3 for M-types (Lisse et al 1999;Britt et al 2002;A'Hearn et al 2005;Fujiwara et al 2006;Carry 2012).…”

Section: Resultsmentioning

confidence: 99%

APO Time-resolved Color Photometry of Highly Elongated Interstellar Object 1I/‘Oumuamua

Bolin

Weaver

Fernández

et al. 2017

ApJL

116

110

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We report on g, r and i band observations of the Interstellar Object 1I/'Oumuamua (1I) taken on 2017 October 29 from 04:28 to 08:40 UTC by the Apache Point Observatory (APO) 3.5m telescope's ARCTIC camera. We find that 1I's colors are g − r = 0.41 ± 0.24 and r − i = 0.23 ± 0.25, consistent with visible spectra (Masiero 2017; Ye et al. 2017;Fitzsimmons et al. 2017) and most comparable to the population of Solar System C/D asteroids, Trojans, or comets. We find no evidence of any cometary activity at a heliocentric distance of 1.46 au, approximately 1.5 months after 1I's closest approach distance to the Sun. Significant brightness variability was seen in the r observations, with the object becoming notably brighter towards the end of the run. By combining our APO photometric time series data with the Discovery Channel Telescope (DCT) data of Knight et al. (2017), taken 20 h later on 2017 October 30, we construct an almost complete lightcurve with a most probable single-peaked lightcurve period of P 4 h. Our results imply a double peaked rotation period of 8.1 ± 0.02 h, with a peak-to-trough amplitude of 1.5 -2.1 mags. Assuming that 1I's shape can be approximated by an ellipsoid, the amplitude constraint implies that 1I has an axial ratio of 3.5 to 10.3, which is strikingly elongated. Assuming that 1I is rotating above its critical break up limit, our results are compatible with 1I having modest cohesive strength and may have obtained its elongated shape during a tidal distortion event before being ejected from its home system.

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Section: Resultsmentioning

confidence: 99%

APO Time-resolved Color Photometry of Highly Elongated Interstellar Object 1I/‘Oumuamua

Bolin

Weaver

Fernández

et al. 2017

ApJL

116

110

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“…As per the description in Lisse et al (1999), the model dust coma was created using the functional form f (Θ) × ρ −n , where ρ is the projected distance on the sky from the nucleus and Θ is the azimuthal angle. In order to compensate for the WISE instrumental effects, the model coma was then convolved with the instrumental PSF appropriate for AWAIC co-added images (see Cutri et al 2012).…”

Section: Nucleusmentioning

confidence: 99%

WISE/NEOWISE PRELIMINARY ANALYSIS AND HIGHLIGHTS OF THE 67P/CHURYUMOV-GERASIMENKO NEAR NUCLEUS ENVIRONS

Bauer

Kramer

Stevenson

et al. 2012

ApJ

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On 2010 January 18-19 and June 28-29, the Wide-field Infrared Survey Explorer (WISE) spacecraft imaged the Rosetta mission target, comet 67P/Churyumov-Gerasimenko. We present a preliminary analysis of the images, which provide a characterization of the dust environment at heliocentric distances similar to those planned for the initial spacecraft encounter, but on the outbound leg of its orbit rather than the inbound. Broadband photometry yields low levels of CO 2 production at a comet heliocentric distance of 3.32 AU and no detectable production at 4.18 AU. We find that at these heliocentric distances, large dust grains with mean grain diameters on the order of a millimeter or greater dominate the coma and evolve to populate the tail. This is further supported by broadband photometry centered on the nucleus, which yield an estimated differential dust particle size distribution with a power-law relation that is considerably shallower than average. We set a 3σ upper limit constraint on the albedo of the large-grain dust at 0.12. Our best estimate of the nucleus radius (1.82 ± 0.20 km) and albedo (0.04 ± 0.01) are in agreement with measurements previously reported in the literature.

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“…The coma removal process involves fitting the coma in azimuthal wedges as a function of the angular distance from the central brightness peak (see Lisse et al 1999Lisse et al , 2009Fernández et al 2000Fernández et al , 2013, and has previously been successfully applied to WISE data . The extracted nucleus signal is then fit to a NEATM, described in more detail in Bauer et al (2015), yielding a 1σ upper bound on the nucleus diameter of 0.7 km, and a 3σ upper bound of 2.2km.…”

Section: Nucleus Sizementioning

confidence: 99%

The Perihelion Emission of Comet C/2010 L5 (WISE)

Kramer

Bauer

Fernández

et al. 2017

ApJ

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The only Halley-type comet discovered by the Wide-Field Infrared Survey Explorer (WISE), C/2010 L5 (WISE), was imaged three times by WISE, and it showed a significant dust tail during the second and third visits (2010 June and July, respectively). We present here an analysis of the data collected by WISE, putting estimates on the comet's size, dust production rate, gas production (CO+CO 2 ) rate, and active fraction. We also present a detailed description of a novel tail-fitting technique that allows the commonly used syndyne-synchrone models to be used analytically, thereby giving more robust results. We find that C/2010 L5ʼs dust tail was likely formed by strong emission, likely in the form of an outburst, occurring when the comet was within a few days of perihelion. Analyses of the June and July data independently agree on this result. The two separate epochs of dust tail analysis independently suggest a strong emission event close to perihelion. The average size of the dust particles in the dust tail increased between the epochs, suggesting that the dust was primarily released in a short period of time, and the smaller dust particles were quickly swept away by solar radiation pressure, leaving the larger particles behind. The difference in CO 2 and dust production rates measured in 2010 June and July is not consistent with "normal" steady-state gas production from a comet at these heliocentric distances, suggesting that much of the detected CO 2 and dust was produced in an episodic event. Together, these conclusions suggest that C/2010 L5 experienced a significant outburst event when the comet was close to perihelion.

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The Nucleus of Comet Hyakutake (C/1996 B2)

Cited by 74 publications

References 38 publications

APO Time-resolved Color Photometry of Highly Elongated Interstellar Object 1I/‘Oumuamua

APO Time-resolved Color Photometry of Highly Elongated Interstellar Object 1I/‘Oumuamua

WISE/NEOWISE PRELIMINARY ANALYSIS AND HIGHLIGHTS OF THE 67P/CHURYUMOV-GERASIMENKO NEAR NUCLEUS ENVIRONS

The Perihelion Emission of Comet C/2010 L5 (WISE)

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