Time series photometry of the dwarf planet ERIS (2003 UB313)

Carraro, G.; Maris, M.; Bertin, D.; Parisi, M. G.

doi:10.1051/0004-6361:20066526

Cited by 23 publications

(15 citation statements)

References 5 publications

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“…We compared these results after a zero-phase correction using a phase coefficient of 0.09 mag/deg (Sheppard 2007). They are consistent with those obtained by other authors (Rabinowitz et al 2006;Sheppard 2007;Carraro et al 2006) within 0.06 mag. They are all plotted together in Fig.…”

Section: Resultssupporting

confidence: 89%

“…According to the rotational phase curves, the spin period of this dwarf planet could be around 14 h or 28 h. For all of these periodicities, the peak-to-peak amplitude of the lightcurve is 0.01 ± 0.01 mag (from sinusoidal fits to the data). These results on amplitude and rotation period are compatible with Carraro et al (2006) who carried out time-series photometry of Eris and estimate a period of about 30 h. Carraro et al (2006) could not determine a precise rotation period because of fewer data points. We believe that the periodicity we derive may be real, but because the amplitude is small, it is possible that the data contained small systematic errors like contamination from faint background stars.…”

Section: Resultssupporting

confidence: 86%

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A study of photometric variations on the dwarf planet (136199) Eris

Duffárd

Ortiz

Santos-Sanz

et al. 2007

A&A

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Context. Eris is the largest dwarf planet currently known in the solar system. Knowledge about its physical parameters is necessary to interpret the characteristics of these kinds of bodies. Aims. The goal of this work is to study Eris' short-term and long-term variability in order to determine the amplitude of the lightcurve, which can be linked to the degree of elongation of the body or to the degree of albedo heterogeneity on the surface of the dwarf planet. In addition, the rotation period can be determined. Methods. CCD photometric observations of the trans Neptunian object Eris in R band on 16 nights spanning two years were carried out using the 1.5 m telescope at Sierra Nevada Observatory (OSN), the 2.5 m Isaac Newton Telescope (INT) telescope at the Roque de los Muchachos Observatory, and the 2.2 m Telescope at Calar Alto Observatory. Results. The time-series analysis leads to indications of a short-term variability whose nature is not clear. It could be real or a result of data-reduction artifacts, such as contamination by close, faint-background stars. The most significant periodicities are 14 h or its double, but other possibilities cannot be ruled out, like a 32 h weaker peak in the periodogram. As for the amplitude of the lightcurve, we get a peak-to-peak variability of 0.01 ± 0.01 mag. The study of the long-term variability indicates that a long rotation period cannot be rejected, but the amplitude would be smaller than 0.06 mag. These results are compatible with a nearly spherical body that has a homogeneous surface.

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Section: Resultssupporting

confidence: 89%

Section: Resultssupporting

confidence: 86%

A study of photometric variations on the dwarf planet (136199) Eris

Duffárd

Ortiz

Santos-Sanz

et al. 2007

A&A

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“…Rotational light-curves of Eris have had little success in obtaining a reliable rotational period (e.g., Carraro et al 2006;or Duffard et al 2008). Roe et al (2008) proposed a rotational period of 1.08 days.…”

Section: Introductionmentioning

confidence: 99%

The spectrum of (136199) Eris between 350 and 2350 nm: results with X-Shooter

Álvarez-Candal

Pinilla-Alonso

Licandro

et al. 2011

A&A

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Context. X-Shooter is the first second-generation instrument for the ESO-Very Large Telescope. It is a spectrograph covering the entire 300−2480 nm spectral range at once with a high resolving power. These properties enticed us to observe the well-known transNeptunian object (136199) Eris during the science verification of the instrument. The target has numerous absorption features in the optical and near-infrared domain that have been observed by different authors, showing differences in these features' positions and strengths. Aims. Besides testing the capabilities of X-Shooter to observe minor bodies, we attempt to constrain the existence of super-volatiles, e.g., CH 4 , CO and N 2 , and in particular we try to understand the physical-chemical state of the ices on Eris' surface. Methods. We observed Eris in the 300−2480 nm range and compared the newly obtained spectra with those available in the literature. We identified several absorption features, measured their positions and depth, and compare them with those of the reflectance of pure methane ice obtained from the optical constants of this ice at 30 K to study shifts in these features' positions and find a possible explanation for their origin. Results. We identify several absorption bands in the spectrum that are all consistent with the presence of CH 4 ice. We do not identify bands related to N 2 or CO. We measured the central wavelengths of the bands and compared to those measured in the spectrum of pure CH 4 at 30 K finding variable spectral shifts. Conclusions. Based on these wavelength shifts, we confirm the presence of a dilution of CH 4 in other ice on the surface of Eris and the presence of pure CH 4 that is spatially segregated. The comparison of the centers and shapes of these bands with previous works suggests that the surface is heterogeneous. The absence of the 2160 nm band of N 2 can be explained if the surface temperature is below 35.6 K, the transition temperature between the alpha and beta phases of this ice. Our results, including the reanalysis of data published elsewhere, point to a heterogeneous surface on Eris.

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“…The rotation period of Eris was considered in several projects, however, there is significant disagreement, ranging from approximately 14 hours to 16 days (e.g. Carraro et al (2006); Sheppard (2007); Maris and Carraro (2008); Duffard et al (2008); Roe et al (2008); Rabinowitz and Owainati (2014)). We consider this parameter to be presently unknown and for simplicity choose a rotation period equal to the orbital period of its satellite Dysnomia, ≈ 16 Earth days (Rabinowitz and Owainati, 2014 (2007)).…”

Section: Volatile Transport On Eris In the Local Collisional Sublimmentioning

confidence: 99%

Ongoing resurfacing of KBO Eris by volatile transport in local, collisional, sublimation atmosphere regime

Hofgartner

Buratti

Hayne

et al. 2019

Icarus

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Kuiper belt object (KBO) Eris is exceptionally bright with a greater visible geometric albedo than any other known KBO. Its infrared reflectance spectrum is dominated by methane, which should form tholins that darken the surface on timescales much shorter than the age of the Solar System.Thus one or more ongoing processes probably maintain its brightness. Eris is predicted to have a primarily nitrogen atmosphere that is in vapor pressure equilibrium with nitrogen-ice and is collisional (not ballistic). Eris's eccentric orbit is expected to result in two atmospheric regimes: (1) a period near perihelion when the atmosphere is global (analogous to the atmospheres of Mars, Triton, and Pluto) and (2) a period near aphelion when only a local * Corresponding author.

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Time series photometry of the dwarf planet ERIS (2003 UB313)

Cited by 23 publications

References 5 publications

A study of photometric variations on the dwarf planet (136199) Eris

A study of photometric variations on the dwarf planet (136199) Eris

The spectrum of (136199) Eris between 350 and 2350 nm: results with X-Shooter

Ongoing resurfacing of KBO Eris by volatile transport in local, collisional, sublimation atmosphere regime

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