Trans-Neptunian Objects as Natural Probes to the Unknown Solar System

Lykawka, Patryk Sofia

doi:10.5047/meep.2012.00103.0121

Cited by 10 publications

(10 citation statements)

References 311 publications

(722 reference statements)

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“…Debris discs, analogues to the Solar system asteroid (O'Brien & Sykes 2011) and Edgeworth-Kuiper (Lykawka 2012) belts, are comprised of objects the size of dwarf planets down to submicron dust particles. Their evolution can be affected strongly by the presence of planets (Hahn & Malhotra 2005;Morbidelli et al 2005;Lykawka et al 2009), therefore one can gain a better understanding of planet formation processes through the study of debris discs with E-mail: nt15@st-andrews.ac.uk a systematic unbiased examination of the frequency of debris discs and statistical analysis of their properties.…”

Section: Introductionmentioning

confidence: 99%

An unbiased study of debris discs around A-type stars with Herschel

Thureau

Greaves

Matthews

et al. 2014

Monthly Notices of the Royal Astronomical Society

123

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The Herschel DEBRIS (Disc Emission via a Bias-free Reconnaissance in the Infrared/Submillimetre) survey brings us a unique perspective on the study of debris discs around main-sequence A-type stars. Bias-free by design, the survey offers a remarkable data set with which to investigate the cold disc properties. The statistical analysis of the 100 and 160 µm data for 86 main-sequence A stars yields a lower than previously found debris disc rate. Considering better than 3σ excess sources, we find a detection rate ≥24 ± 5 per cent at 100 µm which is similar to the debris disc rate around main-sequence F/G/K-spectral type stars. While the 100 and 160 µm excesses slowly decline with time, debris discs with large excesses are found around some of the oldest A stars in our sample, evidence that the debris phenomenon can survive throughout the length of the main sequence (∼1 Gyr). Debris discs are predominantly detected around the youngest and hottest stars in our sample. Stellar properties such as metallicity are found to have no effect on the debris disc incidence. Debris discs are found around A stars in single systems and multiple systems at similar rates. While tight and wide binaries (<1 and >100 au, respectively) host debris discs with a similar frequency and global properties, no intermediate separation debris systems were detected in our sample.

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Section: Introductionmentioning

confidence: 99%

An unbiased study of debris discs around A-type stars with Herschel

Thureau

Greaves

Matthews

et al. 2014

Monthly Notices of the Royal Astronomical Society

123

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show abstract

“…We would dare to say that detailed studies of the outer CR3BP did not seriously begin until the 1990s when the actual "outer" objects were recognized in the solar system, such as the transneptunian objects (TNOs) perturbed by Neptune (e.g. Jewitt and Luu, 1993;Jewitt, 1999;Thomas and Morbidelli, 1996;Lykawka, 2012). Therefore the relevant publications are much fewer than those on the inner CR3BP.…”

Section: Secular Disturbing Function: Outer Casementioning

confidence: 99%

The Lidov-Kozai Oscillation and Hugo von Zeipel

Ito,

Ohtsuka

2019

Preprint

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The circular restricted three-body problem, particularly its doubly averaged version, has been very well studied in celestial mechanics. Despite its simplicity, circular restricted three-body systems are suited for modeling the motion of various objects in the solar system, extrasolar planetary systems, and in many other dynamical systems that show up in astronomical studies. In this context, the so-called Lidov-Kozai oscillation is well known and applied to various objects. This makes the orbital inclination and eccentricity of the perturbed body in the circular restricted three-body system oscillate with a large amplitude under certain conditions. It also causes a libration of the perturbed body's argument of pericenter around stationary points. It is widely accepted that the theoretical framework of this phenomenon was established independently in the early 1960s by a Soviet Union dynamicist (Michail L'vovich Lidov) and by a Japanese celestial mechanist (Yoshihide Kozai). Since then, the theory has been extensively studied and developed. A large variety of studies has stemmed from the original works by Lidov and Kozai, now having the prefix of "Lidov-Kozai" or "Kozai-Lidov." However, from a survey of past literature published in late nineteenth to early twentieth century, we have confirmed that there already existed a pioneering work using a similar analysis of this subject established in that period. This was accomplished by a Swedish astronomer, Edvard Hugo von Zeipel. In this monograph, we first outline the basic framework of the circular restricted three-body problem including typical examples where the Lidov-Kozai oscillation occurs. Then, we introduce what was discussed and learned along this line of studies from the early to mid-twentieth century by summarizing the major works of Lidov, Kozai, and relevant authors. Finally, we make a summary of von Zeipel's work, and show that his achievements in the early twentieth century already comprehended most of the fundamental and necessary formulations that the Lidov-Kozai oscillation requires. By comparing the works of Lidov, Kozai, and von Zeipel, we assert that the prefix "von Zeipel-Lidov-Kozai" should be used for designating this theoretical framework, and not just Lidov-Kozai or Kozai-Lidov. This justifiably shows due respect and appropriately commemorates these three major pioneers who made significant contributions to the progress of modern celestial mechanics.

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“…We will consider just two "classical" scenarios for PX; the one involving a 0.7m ⊕ rock-ice planetoid at some 100 − 175 au (Lykawka and Mukai 2008;Lykawka 2013), and a Tyche-type giant planet (1m J m X 5m J ) at about 10, 000 − 30, 000 au (Matese and Whitmire 2011;Fernández 2011). In the following, we will only consider the range since it turned out that it yields tighter constraints than the range-rate.…”

Section: Px-induced Range Signaturesmentioning

confidence: 99%

“…It is interesting to note that, in recent years, the PX hypothesis is back in vogue (Gomes et al 2006;Lykawka and Mukai 2008;Fernández 2011;Gomes and Soares 2012;Lykawka 2013). As an example, Lykawka (Lykawka 2013) pointed out that the fine orbital structure of the Kuiper belt, the orbits of both the Jovian and the Neptunian Trojans, and, perhaps, the current orbits of the giant planets could be accommodated by the orbital evolution of Mars/Earth-like primordial embryos. They were ultimately scattered by the giant planets; nonetheless, the presently observed features of the trans-Neptunian objects at 40-50 au are optimally satisfied if at least one such primordial planetoid survived in the outskirts of the Solar System.…”

Section: Introductionmentioning

confidence: 99%

“…For the sake of simplicity, we will conventionally denote it as Planet X (PX hereafter); after our analysis, it will turn out that it may quite appropriately be renamed as 1 Telisto. It is interesting to note that, in recent years, the PX hypothesis is back in vogue (Gomes et al 2006;Lykawka and Mukai 2008;Fernández 2011;Gomes and Soares 2012;Lykawka 2013). As an example, Lykawka (Lykawka 2013) pointed out that the fine orbital structure of the Kuiper belt, the orbits of both the Jovian and the Neptunian Trojans, and, perhaps, the current orbits of the giant planets could be accommodated by the orbital evolution of Mars/Earth-like primordial embryos.…”

Section: Introductionmentioning

confidence: 99%

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Perspectives on effectively constraining the location of a massive trans-Plutonian object with the New Horizons spacecraft: a sensitivity analysis

Iorio

2013

Celest Mech Dyn Astr

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The radio tracking apparatus of the New Horizons spacecraft, currently traveling to the Pluto system where its arrival is scheduled for July 2015, should be able to reach an accuracy of 10 m (range) and 0.1 mm s −1 (range-rate) over distances up to 50 au. This should allow to effectively constrain the location of a putative trans-Plutonian massive object, dubbed Planet X (PX) hereafter, whose existence has recently been postulated for a variety of reasons connected with, e.g., the architecture of the Kuiper belt and the cometary flux from the Oort cloud. Traditional scenarios involve a rock-ice planetoid with m X ≈ 0.7m ⊕ at some 100 −200 au, or a Jovian body with m X 5m J at about 10, 000 −20, 000 au; as a result of our preliminary sensitivity analysis, they should be detectable by New Horizons since they would impact its range at a km level or so over a time span six years long. Conversely, range residuals statistically compatible with zero having an amplitude of 10 m would imply that PX, if it exists, could not be located at less than about 4,500 au (m X = 0.7m ⊕ ) or 60,000 au (m X = 5m J ), thus making a direct detection quite demanding with the present-day technologies. As a consequence, it would be appropriate to rename such a remote body as Telisto. Also fundamental physics would benefit from this analysis since certain subtle effects predicted by MOND for the deep Newtonian regions of our Solar System are just equivalent to those of a distant pointlike mass.

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Trans-Neptunian Objects as Natural Probes to the Unknown Solar System

Cited by 10 publications

References 311 publications

An unbiased study of debris discs around A-type stars with Herschel

An unbiased study of debris discs around A-type stars with Herschel

The Lidov-Kozai Oscillation and Hugo von Zeipel

Perspectives on effectively constraining the location of a massive trans-Plutonian object with the New Horizons spacecraft: a sensitivity analysis

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