Observations of 1999 Yc and the Breakup of the Geminid Stream Parent

Kasuga, Toshihiro; Jewitt, David

doi:10.1088/0004-6256/136/2/881

Cited by 54 publications

(40 citation statements)

References 51 publications

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“…The Geminid meteoroids show extreme diversity in their Na abundance, from strong depletion to near Sun-like Na content (Harvey 1973;Borovička et al 2005;Kasuga et al 2005). Presumably, this compositional diversity reflects different thermal modification on Phaethon (or perhaps the larger sized precursor body) itself Kasuga et al 2006;Ohtsuka et al 2006;Kasuga & Jewitt 2008;Capek & Borovička 2009;Kasuga 2009;Ohtsuka et al 2009). For the Quadrantid meteoroids, the measured line intensity ratios show that Na is less depleted than in the majority of Geminid meteoroids (Koten et al 2006;Borovička et al 2010).…”

Section: Discussionmentioning

confidence: 99%

Physical Observations of (196256) 2003 Eh1, Presumed Parent of the Quadrantid Meteoroid Stream

Kasuga

Jewitt

2015

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The near-Earth asteroid (196256) 2003 EH1 has been suggested to have a dynamical association with the Quadrantid meteoroid stream. We present photometric observations taken to investigate the physical character of this body and to explore its possible relation to the stream. We find no evidence for ongoing mass loss. A model fitted to the point-like surface brightness profile at 2.1 AU limits the fractional contribution to the integrated brightness by the near-nucleus coma to 2.5%. Assuming an albedo equal to those typical of cometary nuclei (p R = 0.04), we find that the effective nucleus radius is r e = 2.0 ± 0.2 km. Time-resolved R-band photometry can be fitted by a two-peaked light curve having a rotational period of 12.650 ± 0.033 hr. The range of the light curve, Δm R = 0.44 ± 0.01 mag, is indicative of an elongated shape having an axis ratio of ∼1.5 projected into the plane of the sky. The asteroid shows colors slightly redder than the Sun, being comparable with those of C-type asteroids. The limit to the mass loss rate set by the absence of the resolved coma is 2.5 × 10 −2 kg s −1 , corresponding to an upper limit on the fraction of the surface that could be sublimating water ice f A  10 −4 . Even if sustained over the 200-500 year dynamical age of the Quadrantid stream, the total mass loss from 2003 EH1 would be too small to supply the reported stream mass (10 13 kg), implying either that the stream has another parent or that mass loss from 2003 EH1 is episodic.

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Section: Discussionmentioning

confidence: 99%

Physical Observations of (196256) 2003 Eh1, Presumed Parent of the Quadrantid Meteoroid Stream

Kasuga

Jewitt

2015

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“…This object is dynamically associated with the Geminid meteor stream (e.g., Williams & Wu 1993) and with several other small asteroids including 2005 UD (Ohtsuka et al 2006;Konoshita et al 2007) and 1999 YC (Ohtsuka et al 2008;Kasuga & Jewitt 2008). All these objects may be related to a precursor body that disintegrated ∼10 3 yr ago (Ohtsuka et al 2006).…”

Section: Observations Of Active Asteroidsmentioning

confidence: 92%

The Active Asteroids

Jewitt

2012

The Astronomical Journal

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287

244

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Some asteroids eject dust, unexpectedly producing transient, comet-like comae and tails. First ascribed to the sublimation of near-surface water ice, mass-losing asteroids (also called "main-belt comets") can in fact be driven by a surprising diversity of mechanisms. In this paper, we consider 11 dynamical asteroids losing mass, in nine of which the ejected material is spatially resolved. We address mechanisms for producing mass loss including rotational instability, impact ejection, electrostatic repulsion, radiation pressure sweeping, dehydration stresses, and thermal fracture, in addition to the sublimation of ice. In two objects (133P and 238P) the repetitive nature of the observed activity leaves ice sublimation as the only reasonable explanation, while in a third ((596) Scheila), a recent impact is the cause. Another impact may account for activity in P/2010 A2, but this tiny object can also be explained as having shed mass after reaching rotational instability. Mass loss from (3200) Phaethon is probably due to cracking or dehydration at extreme (∼1000 K) perihelion temperatures, perhaps aided by radiation pressure sweeping. For the other bodies, the mass-loss mechanisms remain unidentified, pending the acquisition of more and better data. While the active asteroid sample size remains small, the evidence for an astonishing diversity of mass-loss processes in these bodies is clear.

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“…Second, we derived a parameter η defined as the ratio of the coma cross section C c to the nucleus cross section C n . At optical wavelengths, η is proportional to the ratio of the flux density scattered by the coma, I c , to the flux density scattered by the nucleus cross section, I n , which enables us to characterize the contribution of dust particles in the coma (Luu & Jewitt 1992;Hsieh & Jewitt 2005;Kasuga & Jewitt 2008), that is,…”

Section: Dust Mass-loss Ratementioning

confidence: 99%

Comet 17p/Holmes: Contrast in Activity Between Before and After the 2007 Outburst

Ishiguro¹,

Kim²,

Kim³

et al. 2013

ApJ

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A Jupiter-family comet, 17P/Holmes, underwent outbursts in 1892 and 2007. In particular, the 2007 outburst is known as the greatest outburst over the past century. However, little is known about the activity before the outburst because it was unpredicted. In addition, the time evolution of the nuclear physical status has not been systematically studied. Here we study the activity of 17P/Holmes before and after the 2007 outburst through optical and mid-infrared observations. We found that the nucleus highly depleted its near-surface icy component before but became activated after the -3 -2007 outburst. Assuming a conventional 1-µm-sized grain model, we derived a surface fractional active area of 0.58% ± 0.14% before the outburst whereas it was enlarged by a factor of ∼50 after the 2007 outburst. We also found that large (≥1 mm) particles could be dominant in the dust tail observed around aphelion. Based on the size of the particles, the dust production rate was 170 kg s −1 at the heliocentric distance r h = 4.1 AU, suggesting that the nucleus still held active status around the aphelion passage. The nucleus color was similar to that of the dust particles and average for a Jupiter-family comet but different from most Kuiper Belt objects, implying that the color may be inherent to icy bodies in the solar system. On the basis of these results, we concluded that more than 76 m surface materials were blown off by the 2007 outburst.

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Observations of 1999 Yc and the Breakup of the Geminid Stream Parent

Cited by 54 publications

References 51 publications

Physical Observations of (196256) 2003 Eh1, Presumed Parent of the Quadrantid Meteoroid Stream

Physical Observations of (196256) 2003 Eh1, Presumed Parent of the Quadrantid Meteoroid Stream

The Active Asteroids

Comet 17p/Holmes: Contrast in Activity Between Before and After the 2007 Outburst

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