Abstract:Aims. We studied the rotational properties of the dwarf planet Makemake. Methods. The photometric observations were carried out at different telescopes between 2006 and 2017. Most of the measurements were acquired in BVRI broad-band filters of a standard Johnson-Cousins photometric system. Results. We found that Makemake rotates more slowly than was previously reported. A possible lightcurve asymmetry suggests a double-peaked period of P = 22.8266±0.0001 h. A small peak-to-peak lightcurve amplitude in R-filter… Show more
“…The averaged V − R colour indices obtained in this work and the corresponding literature data are given in Table 2. The V − R values calculated from different periods of the observations for Haumea and Makemake are scattered, while [30] and [12] discuss that these values do not considerably change. For Makemake, the V − R result 0.41 ± 0.02 obtained in [12] is inside our range of values.…”
Section: Discussionmentioning
confidence: 99%
“…The V − R values calculated from different periods of the observations for Haumea and Makemake are scattered, while [30] and [12] discuss that these values do not considerably change. For Makemake, the V − R result 0.41 ± 0.02 obtained in [12] is inside our range of values. For other objects, our V − R colours do not show close agreement with the reference values in Table 2.…”
Section: Discussionmentioning
confidence: 99%
“…The paper [12] included the new values of the absolute magnitudes of Makemake, H R = −0.388±0.02 in the R filter, and the value given in Table 2 in the V filer. It is an example of the use of a 0.7-m telescope (R filter) as a part of the instrumentation for the long-term photometric monitoring of a faint object, which is a general method of obtaining the absolute magnitude.…”
Section: Discussionmentioning
confidence: 99%
“…Visible and near-infrared spectral observations of Makemake showed that this object has an overall homogeneous surface [31]. Recent results of the long-term monitoring of Makemake suggested that it has an almost spherical shape and estimated its rotational period as 22.826 hours [12]. Makemake passed aphelion in 1992.…”
In this work we focused on observations of six trans-Neptunian objects (TNOs) whose apparent magnitudes are brighter than 20m. We present the results of astrometric and photometric observations of (134340) Pluto, (136108) Haumea, (136472) Makemake, (136199) Eris, (90482) Orcus, and (20000) Varuna obtained at the Kyiv comet station (Code MPC 585) in 2017-2019. For observations we used the 0.7-m (f/4) reflector AZT-8 with FLI PL4710 CCD camera and filters of Johnson-Cousins photometric system. From our images we measured the objects' astrometric positions, calculated apparent magnitudes in the BVRI (mostly R) bands using aperture photometry method, and found absolute magnitudes together with the colour indices in several bands. Analysing our results, we investigate the limitation on the astrometry and photometry of faint objects with the 0.7-m telescope.
“…The averaged V − R colour indices obtained in this work and the corresponding literature data are given in Table 2. The V − R values calculated from different periods of the observations for Haumea and Makemake are scattered, while [30] and [12] discuss that these values do not considerably change. For Makemake, the V − R result 0.41 ± 0.02 obtained in [12] is inside our range of values.…”
Section: Discussionmentioning
confidence: 99%
“…The V − R values calculated from different periods of the observations for Haumea and Makemake are scattered, while [30] and [12] discuss that these values do not considerably change. For Makemake, the V − R result 0.41 ± 0.02 obtained in [12] is inside our range of values. For other objects, our V − R colours do not show close agreement with the reference values in Table 2.…”
Section: Discussionmentioning
confidence: 99%
“…The paper [12] included the new values of the absolute magnitudes of Makemake, H R = −0.388±0.02 in the R filter, and the value given in Table 2 in the V filer. It is an example of the use of a 0.7-m telescope (R filter) as a part of the instrumentation for the long-term photometric monitoring of a faint object, which is a general method of obtaining the absolute magnitude.…”
Section: Discussionmentioning
confidence: 99%
“…Visible and near-infrared spectral observations of Makemake showed that this object has an overall homogeneous surface [31]. Recent results of the long-term monitoring of Makemake suggested that it has an almost spherical shape and estimated its rotational period as 22.826 hours [12]. Makemake passed aphelion in 1992.…”
In this work we focused on observations of six trans-Neptunian objects (TNOs) whose apparent magnitudes are brighter than 20m. We present the results of astrometric and photometric observations of (134340) Pluto, (136108) Haumea, (136472) Makemake, (136199) Eris, (90482) Orcus, and (20000) Varuna obtained at the Kyiv comet station (Code MPC 585) in 2017-2019. For observations we used the 0.7-m (f/4) reflector AZT-8 with FLI PL4710 CCD camera and filters of Johnson-Cousins photometric system. From our images we measured the objects' astrometric positions, calculated apparent magnitudes in the BVRI (mostly R) bands using aperture photometry method, and found absolute magnitudes together with the colour indices in several bands. Analysing our results, we investigate the limitation on the astrometry and photometry of faint objects with the 0.7-m telescope.
“…As an example, we cite Ceres, whose oblate shape is well known from stellar occultations (Gomes-Júnior et al 2015) and the DAWN spacecraft visit (Russell et al 2016) while it exhibits a lowamplitude double-peaked rotational light-curve that is caused by albedo features (Chamberlain et al 2007). In the trans-neptunian region, Makemake is also a clear example of an oblate body with a low-amplitude double-peaked light-curve (Hromakina et al 2019).…”
Context. We present results from the first recorded stellar occultation by the large trans-Neptunian object (174567) Varda that was observed on September 10, 2018. Varda belongs to the high-inclination dynamically excited population, and has a satellite, Ilmarë, which is half the size of Varda.
Aims. We determine the size and albedo of Varda and constrain its 3D shape and density.
Methods. Thirteen different sites in the USA monitored the event, five of which detected an occultation by the main body. A best-fitting ellipse to the occultation chords provides the instantaneous limb of the body, from which the geometric albedo is computed. The size and shape of Varda are evaluated, and its bulk density is constrained using Varda’s mass as is known from previous works.
Results. The best-fitting elliptical limb has semi-major (equatorial) axis of (383 ± 3) km and an apparent oblateness of 0.066 ± 0.047, corresponding to an apparent area-equivalent radius R′equiv = (370±7) km and geometric albedo pv = 0.099 ± 0.002 assuming a visual absolute magnitude HV = 3.81 ± 0.01. Using three possible rotational periods for the body (4.76, 5.91, and 7.87 h), we derive corresponding MacLaurin solutions. Furthermore, given the low-amplitude (0.06 ± 0.01) mag of the single-peaked rotational light-curve for the aforementioned periods, we consider the double periods. For the 5.91 h period (the most probable) and its double (11.82 h), we find bulk densities and true oblateness of ρ = (1.78 ± 0.06) g cm−3, ɛ = 0.235 ± 0.050, and ρ = (1.23 ± 0.04) g cm−3, ɛ = 0.080 ± 0.049. However, it must be noted that the other solutions cannot be excluded just yet.
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