1 INTRODUCTION
At the beginning of the 21st century and given the knowledge acquired during the 20th century as a result of the investigations of stars in the main sequence of the H-R diagram has become clear that approximately a half of the stars in our galaxy belong to binary or multiple star systems (Duquennoy & Mayor Reference Duquennoy and Mayor1991; Kononovich & Moroz Reference Kononovich and Moroz2004). Taking this observational fact into account, the following questions arise: Is the Sun the only star in the Solar System? Does it have a companion?
A number of recent observational facts have provided a preliminary answer to the questions posed above almost discarding the existence of a stellar or substellar companion to the Sun. Data from the WISE infrared space telescope (Luhman Reference Luhman2014) showed no evidence of a planet the size of Saturn out to 28 000 AU, Jupiter out to 82 000 AU, or a Jupiter-sized brown dwarf out to 26 000 AU at the locations suggested by Matese & Whitmire (Reference Matese and Whitmire1986). The version of the Nemesis hypothesis (Davis, Hut, & Muller Reference Davis, Hut and Muller1984) assuming that the companion of the Sun was a common M-dwarf star has been ruled out by full sky surveys, the latest of which is the NASA WISE mid-IR survey (Luhman Reference Luhman2014). However, the alternative version of the Nemesis hypothesis (Whitmire & Jackson Reference Whitmire and Jackson1984) assuming that the Sun’s companion was a substellar object with a mass between 0.07 and 0.0002 solar masses may still be viable. The lower end of this mass range is not ruled out by WISE or any other full sky survey given the fact that the object would likely be closer to aphelion today (Whitmire Reference Whitmire2016). Moreover, there is still room for the existence of trans-Plutonian planets even ten times as massive as the Earth at a distance of more than 195 AU from the Sun (Trujillo & Sheppard Reference Trujillo and Sheppard2014; de la Fuente Marcos & de la Fuente Marcos Reference de la Fuente Marcos and de la Fuente Marcos2014; de la Fuente Marcos, de la Fuente Marcos, & Aarseth Reference de la Fuente Marcos, de la Fuente Marcos and Aarseth2015; Batygin & Brown Reference Batygin and Brown2016).
Now that the existence of another stellar, substellar,or Jovian-like planetary body in the Solar System is very unlikely, if other massive bodies exist they must be planetary in nature and no more massive than about ten Earth masses being located at a distance of more than 150 AU from the Sun. These putative cold and dark objects located at large distances from the Sun are difficult to detect even in the infrared region of the electromagnetic spectrum. In some cases, they could have probably been detected by past surveys (Batygin & Brown Reference Batygin and Brown2016; Linder & Mordasini Reference Linder and Mordasini2016). These dark bodies moving very slowly at the Solar System periphery have huge orbital periods and the chances to detect them using conventional techniques are remote. Because of this, the study of gravitational perturbations and stellar occultations produced by such massive objects, and the analysis of their effects on the light coming from distant stars have become crucial methods to be used in their detection (Roques, Moncuquet, & Sicardy Reference Roques, Moncuquet and Sicardy1987; Gaudi & Sackett Reference Gaudi and Sackett2000; Cooray Reference Cooray2002; Gaudi & Bloom Reference Gaudi and Bloom2005; Bickerton, Kavelaars, & Welch Reference Bickerton, Kavelaars and Welch2008; Heyl Reference Heyl2010; Zhdanov & Gorpinchenko Reference Zhdanov and Gorpinchenko2012).
The possibility of detecting a far away and dark massive body indirectly by means of its effects on the light coming from distant stars could be the basis of a new approach to the search for a trans-Plutonian planet at the Solar System periphery by using the gravitational lensing method (GLM). The GLM was first mentioned by the Russian physicist O. Chwolson (Chwolson Reference Chwolson1924) and then studied quantitatively by A. Einstein (Einstein Reference Einstein1936). It is based on the effect of gravitational lensing consisting in bending of light beams coming from distant stars by a dark and massive point-like object (lens). Two or more images of a source are formed by the lens. If these separate images are resolved by the telescope, then it is called strong lensing. Otherwise, it is called gravitational microlensing and in this case, the gravitational field of the dark and massive point-like object affects starlight resulting in a great increase of the brightness of the stars. The gravitational microlensing effect is the basis of the gravitational microlensing method (GMM) which has been first proposed by B. Paczynski (Paczynski Reference Paczynski1986a, Reference Paczynski1986b). The realisation of the method in practice has taken place at the beginning of the 21st century (Zhu et al. Reference Zhu2015) and in the near future, it may be used to search for a putative dark massive planet at the edge of the Solar System.
The main purpose of this work is to determine the basic physical properties of a massive dark body (this can be a brown dwarf—Nemesis, a giant planet as massive or more massive than Jupiter—Tyche, or a trans-Plutonian planet as massive or more massive than Earth but less massive than Neptune—Planet Nine (P9) or any other trans-Plutonian planet) which may exist at the Solar System periphery and to perform a quantitative analysis of the possibility of detection of such a body using the GLM.
2 ABOUT THE FACTS SUPPORTING THE EXISTENCE OF TRANS-PLUTONIAN PLANETS
In this section, we present the most important facts supporting indirectly the hypothesis of the existence of a massive dark planet at the Solar System periphery.
I. As explained above, approximately 50% of all main sequence stars are part of double or multiple stars systems (Duquennoy & Mayor Reference Duquennoy and Mayor1991; Kononovich & Moroz Reference Kononovich and Moroz2004). Based on this observational fact, it had been suggested that the Sun may have a gravitationally bound companion star, i.e., the Sun could be part of a binary system. However, recent WISE space telescope observational findings (Luhman Reference Luhman2014) have decreased the credibility of this hypothesis to a minimum level. Data from the WISE infrared space telescope (Luhman Reference Luhman2014) showed no evidence of a Jupiter-sized brown dwarf out to 26 000 AU at the locations suggested by Matese & Whitmire (Reference Matese and Whitmire1986). Only the lower end of the mass range proposed in Whitmire and Jackson’s Nemesis hypothesis (Whitmire & Jackson Reference Whitmire and Jackson1984), i.e., a brown dwarf companion to the Sun with a mass of 0.0002 solar masses, has not yet been ruled out by NASA WISE or any other full sky survey (Whitmire Reference Whitmire2016).
II. Palaeontologists J. Sepkoski and D. M. Raup (Raup & Sepkoski Reference Raup and Sepkoski1984) published the results of the analysis of geological layers, corresponding to the different eras, spanning the last 250 Myr. They found 12 events corresponding to sharp increases in mortality of living organisms on Earth. The time interval between two of these events is about 27 Myr (see Figure 1). Raup and Sepkoski concluded that such events (including the alleged disappearance of the dinosaurs 65 Myr ago) happened regularly and could have an extraterrestrial origin, in particular, a gravitational disturbance in the Oort cloud of comets, caused by the presence of a massive dark body in the outskirts of the Solar System. Gravitational perturbations generated by such a dark body may have led to a cometary migration to the inner Solar System and some of these perturbed comets, or a near-Earth asteroid whose orbit was distorted by their presence, could have collided with Earth. A putative asteroidal or cometary impact could have caused the global catastrophe that led to the demise of a great amount of living organisms on Earth. Recently, the topic of the periodic mass extinctions and the Planet X hypothesis has been revisited (Whitmire Reference Whitmire2016). D. P. Whitmire concludes that the Planet X hypothesis can explain the 27 Myr periodicity in the fossil extinction record. In this case, the period in question is associated with the perihelion precession of the inclined orbit of a trans-Neptunian planet (more massive than Earth but less massive than Neptune). The existence of such a trans-Neptunian super-Earth planet has been proposed to explain the observational fact that inner Oort cloud objects such as Sedna and 2012 VP113 have perihelia that lie near the ecliptic plane (Trujillo & Sheppard Reference Trujillo and Sheppard2014; de la Fuente Marcos & de la Fuente Marcos Reference de la Fuente Marcos and de la Fuente Marcos2014; Iorio Reference Iorio2014; de la Fuente Marcos et al. Reference de la Fuente Marcos, de la Fuente Marcos and Aarseth2015; Batygin & Brown Reference Batygin and Brown2016).
Mortality curve of living organisms on Earth, according to Raup & Sepkoski (Reference Raup and Sepkoski1984).
III. Long-term studies of comets have shown that new comets, coming to us from the Solar System periphery, appear regularly: In some years, the number of comets is significantly higher than in others. Most of the comets are approaching to the Earth at perihelia coming from the Oort cloud (Yarris Reference Yarris1987). The periodicity of such comets appears to be directly related to the periodicity in movement of an unknown massive celestial body that may exist in the outskirts of the Solar System.
IV. Pluto, Eris, Sedna, and other trans-Neptunian and extreme trans-Neptunian objects (ETNOs) have very elongated orbits and large values of orbit inclinations to the plane of the ecliptic. In the case of Sedna, its extremely elliptical orbit as well as its dynamical evolution cannot be convincingly explained by the current model of the Solar System that includes only eight major planets revolving around the Sun (Brown Reference Brown2004). However, these extremely elongated orbits and high inclinations can be easily explained by the existence of a massive celestial body located at the Solar System periphery. From such a vantage location, a putative massive dark planet may induce gravitational perturbations on the trans-Neptunian objects (Gomes, Matese, & Lissauer Reference Gomes, Matese and Lissauer2006).
V. The study of the circumstellar discs of the stars HD53143 and HD139664 with HST (Hubble space telescope) has shown that both discs appear to be in a stable state of equilibrium (Kalas et al. Reference Kalas, Graham, Clampin and Fitzgerald2006). The dust disk of each star is divided into two zones. One of them is a wide belt with a gradually decreasing density of matter, starting with r ⩾ 50 AU from the star. The second disc is located in the range of 20–30 AU from the star and has a distinct outer edge, the density of material in the disk falls sharply here. This may indicate the presence of a companion star or planet. The object’s orbit runs along the outer edge of the disc. It constantly cuts the edge of the circumstellar disc, protecting it from erosion. Similar effects are observed in the rings of Saturn. The existence of these circumstellar discs, even considering that they may include belts similar to the Kuiper belt, has some implications for the case of the Solar System, despite of the physical properties of the stars HD53143 and HD139664 are slightly different than the ones corresponding to the Sun. Recently, S. J. Kenyon and B. C. Bromley have shown (Kenyon & Bromley Reference Kenyon and Bromley2015, Reference Kenyon and Bromley2016) how it is possible—for mechanisms acting on a stellar protoplanetary disc—to form planets as massive or even 15 times as massive as the Earth at distances within the range 125–750 AU from a solar-type star. Moreover, observational inference of extrasolar planetary systems such as HR 8799 (Marois et al. Reference Marois2008) suggests that planets can indeed occupy exceptionally wide orbits.
VI. The results of Monte Carlo simulations (de la Fuente Marcos & de la Fuente Marcos Reference de la Fuente Marcos and de la Fuente Marcos2014) and numerical integrations using an N-body model applied to comet 96P/Machholz 1 (de la Fuente Marcos et al. Reference de la Fuente Marcos, de la Fuente Marcos and Aarseth2015) strongly suggest that trans-Plutonian planets may exist. According to these authors, beyond the orbit of Pluto at distances of about 205–264, 346–416, 610–692, and 972–1001 AU from the Sun—a number of massive planets may be located.
VII. According to new ALMA (Atacama Large Millimeter/submillimeter Array) observational findings (Liseau et al. Reference Liseau2015; Vlemmings et al. Reference Vlemmings, Ramstedt, Maercker and Davidsson2015), two new objects of the Solar System have been discovered. One of them is a fast moving single object (with proper motion 87 arcsec yr− 1), named Gna, that could be a large Centaur with a size within the range 220–880 km at a distance of 12–20 AU if it is gravitationally bound or a low-mass brown dwarf beyond 4 000 AU if it is not gravitationally bound (Vlemmings et al. Reference Vlemmings, Ramstedt, Maercker and Davidsson2015). The nature of this object is not yet clear, its geocentric distance is unknown. The other object shares the high proper motion of alpha Centauri and has a prograde motion (Liseau et al. Reference Liseau2015). According to Liseau et al., the object could be a super-Earth (with a radius one and a half times that of the Earth and located at a distance of about 300 AU from the Sun) or a super-cool brown dwarf (at a distance of about 20 000 AU). Considering that WISE space telescope infrared observations found no evidence of a planet the size of Saturn out to 28 000 AU, Jupiter out to 82 000 AU, or a Jupiter-sized brown dwarf out to 26 000 AU at the locations suggested by Matese & Whitmire (Luhman Reference Luhman2014), the first option, i.e., the existence of a trans-Plutonian planet 2–15 times as massive as the Earth at a distance of approximately 300 AU from the Sun, is the most probable one. However, it must be emphasised here that both discoveries by ALMA are no more than unconfirmed tentative candidates to be members of the Solar System. They may well correspond to false or spurious detections until proven otherwise. Clearly, more observations of these objects are needed to confirm their existence.
VIII. Very recently, K. Batygin and M. E. Brown (Batygin & Brown Reference Batygin and Brown2016; Brown & Batygin Reference Brown and Batygin2016) have found that the observed orbital alignment of the ETNOs can be maintained by a distant, eccentric trans-Plutonian planet with a mass close to that of Neptune or lower lying approximately in the same orbital plane defined by some of the ETNOs, i.e., with inclination of approximately 30°, and with perihelion 180° away from the perihelia of the ETNOs. In addition to accounting for the observed orbital alignment, the existence of such a planet naturally explains the presence of high-perihelion Sedna-like objects, as well as the known collection of high semi-major axis objects with inclinations between 60° and 150° whose origin was previously unclear. However, although this hypothesis has been successful in generating a distant population of small bodies whose orbits exhibit alignment in physical space, there are observational aspects of the distant Kuiper Belt that the P9 hypothesis is unable to address. Specifically, the apparent clustering of arguments of perihelia near argument of perihelion zero in the 150–250 AU region remains somewhat puzzling (Batygin & Brown Reference Batygin and Brown2016). To explain such a feature, another massive perturber, perhaps with mass within the range 2–15 Earth masses, at a distance of 264 AU from the Sun in a moderately eccentric orbit with low inclination could be required (de la Fuente Marcos et al. Reference de la Fuente Marcos, de la Fuente Marcos and Aarseth2015).
On the other hand, to explain the unusual orbital distribution of distant Kuiper belt objects (KBOs) or ETNOs, Fienga et al. (Reference Fienga, Laskar, Manche and Gastineau2016) have advocated the existence of a super-Earth planet in the outer Solar System, based on the P9 hypothesis proposed by Batygin & Brown (Reference Batygin and Brown2016). Making use of the most sensitive data set, the Cassini radio ranging data and the INPOP planetary ephemerides model (Fienga et al. Reference Fienga, Manche, Laskar and Gastineau2008, Reference Fienga2009, Reference Fienga2011), Fienga et al. (Reference Fienga, Laskar, Manche and Gastineau2016) have shown that a trans-Plutonian planet with mass 10 Earth masses, moving along an orbit with a semi major axis of 700 AU and an eccentricity of 0.6, may exist if its true anomaly does not belong to the interval [− 130°, −100°] and [− 65°, 85°]. Moreover, Fienga et al. (Reference Fienga, Laskar, Manche and Gastineau2016) point out the most probable position of P9 given by a true anomaly 117.8°+ 11°− 10°. Using Cassini data up to the epoch 2014.4 and the extrapolated Cassini data up to 2020, Fienga et al. (Reference Fienga, Laskar, Manche and Gastineau2016) were able to identify new and more stringent restrictions on the range of possible values for the true anomaly. If the Cassini mission is extended until 2020, it would thus allow to state for the non-existence of P9 on the intervals of true anomaly given by [− 132°, 106.5°]. Therefore, the corresponding range of available heliocentric distances for P9 is constrained by Cassini data to 549–1120 AU, being q = 280 AU the perihelion distance of P9.
3 PHYSICAL PROPERTIES OF NEMESIS, TYCHE, PLANET NINE, AND ANY OTHER TRANS-PLUTONIAN PLANET
Whitmire & Jackson (Reference Whitmire and Jackson1984) and Davis et al. (Reference Davis, Hut and Muller1984) first proposed the hypothesis of the existence of a stellar companion to the Sun which moves with it around a common centre of mass and together form a binary star (see e.g., Muller Reference Muller2002). It was named NemesisFootnote 1 . Since then, other scientists have supported the hypothesis of Whitmire, Jackson, and Davis, and they have accomplished a theoretical analysis of the properties of the object (Bhalerao & Vahia Reference Bhalerao and Vahia2005). However, after the publication of the results obtained by the WISE space telescope (Luhman, Reference Luhman2014) that found no evidence of a Jupiter-sized brown dwarf out to 26 000 AU at the locations suggested by Matese & Whitmire (Reference Matese and Whitmire1986), the chances for the existence of Nemesis are very slim. However, a brown dwarf companion to the Sun with a mass of 0.0002 solar masses, which corresponds to the lower end of the mass range proposed by Whitmire and Jackson (Whitmire & Jackson Reference Whitmire and Jackson1984), has not yet been ruled out by NASA WISE or any other full sky survey (Whitmire Reference Whitmire2016).
Table 1 shows a summary of numerical values of basic characteristics of Nemesis and its orbit that have been used in this research. We propose a permissible range of mass values (which is expressed in solar masses, M⊙ = 1.989 ×1030 kg) and the effective temperature of Nemesis’ surface corresponding to a brown dwarf, according to Burrows et al. (Reference Burrows, Hubbard, Saumon and Lunine1993). We also take into account that a typical brown dwarf has a radius approximately equal to Jupiter’s radius
$\mathfrak {R}_{\mathrm{N}} \approx R_{\mathrm{J}}$
.Footnote
2
Basic properties of Nemesis and its orbit.
Matese et al. (Reference Matese, Whitmire and Whitman2011) proposed the hypothesis of the existence of a massive cosmic body, a gas giant planet, in the Oort cloud. It was named TycheFootnote 3 . Data analysis of long-term observations of the orbits of comets approaching the Sun led the research team to the conclusion that about 20% of the comets falling into the inner part of the Solar system are attracted by the gravitational force of a massive cosmic object in the Oort cloud. According to these authors, the massive object would have a mass at least 1.4 times higher than Jupiter’s mass. But if it was a star, the percentage of comets, captured by the gravitational field, would be much higher. However, after the publication of the results obtained by the WISE space telescope (Luhman, Reference Luhman2014) that found no evidence of a Jupiter-sized brown dwarf out to 26 000 AU at the locations suggested by Matese & Whitmire (Reference Matese and Whitmire1986), the possibility of the existence of Tyche is more remote than ever.
Table 2 shows a summary of numerical values of Tyche’s basic physical properties. As for the range of possible values for Tyche’s mass (expressed in Jupiter masses—M J), a range of values allowed for planets like Jupiter (Jovian planets) is used (Burrows et al. Reference Burrows, Hubbard, Saumon and Lunine1993). We have taken into account that the orbit of Tyche should not go beyond the solar Hill sphere (which external radius is at least 1.20 ×105 AU) to determine the allowable heliocentric distances (see inequality (9) in Table 2). The lower limit for the semi-major axis of the orbit of Tyche is determined by the internal radius of the Oort cloud, based on the assumption that the orbit of Tyche is fully included in the Oort cloud.
Basic properties of Tyche and its orbit.
Trujillo & Sheppard (Reference Trujillo and Sheppard2014) first proposed the existence of a trans-Plutonian planet to explain the orbital behaviour of the distant KBO 2012 VP113. They compared the orbit of 2012 VP113 with that of the dwarf planet Sedna and concluded that the orbits of these objects suggest that a massive object, a planet heavier than Earth, could exist at around 250 AU moving along an almost circular orbit. An alternative scenario, the P9 hypothesis, has been proposed by Batygin & Brown (Reference Batygin and Brown2016). These authors argue that the gravitational perturbation generated by a massive outer planet moving along an eccentric and moderately inclined orbit with semi-major axis of 700 AU (P9) would be the most likely explanation for the perihelia clustering of the orbits of six distant KBOs.
Tables 3 and 4 show a summary of numerical values of the basic physical properties of P9 and any other trans-Plutonian planet with different but plausible values. The majority of the parameter ranges have been taken from Batygin & Brown (Reference Batygin and Brown2016). For comparison, we have also provided the ranges in mass, radius, perihelion distance, semi-major axis, and heliocentric distance for P9 according to Brown & Batygin’s more recent work (Brown & Batygin Reference Brown and Batygin2016). We have also taken into account the results in de la Fuente Marcos & de la Fuente Marcos (Reference de la Fuente Marcos and de la Fuente Marcos2014), Iorio (Reference Iorio2014), Trujillo & Sheppard (Reference Trujillo and Sheppard2014), de la Fuente Marcos et al. (Reference de la Fuente Marcos, de la Fuente Marcos and Aarseth2015), Liseau et al. (Reference Liseau2015), Fienga et al. (Reference Fienga, Laskar, Manche and Gastineau2016), Fortney et al. (Reference Fortney2016), Ginzburg et al. (Reference Ginzburg, Sari and Loeb2016), Kenyon & Bromley (Reference Kenyon and Bromley2016), and Linder & Mordasini (Reference Linder and Mordasini2016) to extend the ranges of mass (from one to fifteen Earth masses,
$M_{\bigoplus }$
), radius (from one to four Earth radii,
$R_{\bigoplus }$
) and available heliocentric distances (from 200 to 2 000 AU) of any other trans-Plutonian planet. The orbital period of P9 has been taken as approximately equal to 18 520 yr, following Batygin & Brown (Reference Batygin and Brown2016). In the case of a trans-Plutonian planet, other than P9, the range of possible values for the orbital period goes from 2 828 to 89 443 yr.
Basic properties of Planet Nine (P9) and its orbit.
Basic properties of a trans-Plutonian planet (TP), other than P9, and its orbit.
4 QUANTITATIVE ANALYSIS OF THE FEASIBILITY OF THE DETECTION OF NEMESIS, TYCHE, AND TRANS-PLUTONIAN PLANETS USING GLM
4.1. Deflection angle in the gravitational field of Nemesis, Tyche, and a trans-Plutonian planet
We consider the problem of the possibility of detecting either Nemesis, Tyche, or a trans-Plutonian planet that is playing the role of a gravitational lens using the following assumptions about the gravitational lens and the electromagnetic radiation coming from the background source.
-
1. A gravitational lens (Nemesis, Tyche, or a trans-Plutonian planet less massive than Neptune) is a spherical body of radius
$\mathfrak {R}$
and mass
$\mathfrak {M}$
with a spherically symmetric distribution of matter. Given its size and distance from the observer, the gravitational lens has a negligible angular dimension. -
2. The gravitational influence of the major planets and other bodies of the Solar System on the light beams coming from the background source in the vicinity of the gravitational lens will be neglected.
-
3. Absorption of light by the interplanetary medium will also be neglected.
The electromagnetic radiation of the background star (source) can be considered as the photon beam. The dynamic photon mass m γ is determined using the Einstein’s formula:
$$\begin{equation}
m_{\gamma } = \frac{E_{\gamma }}{c^2} = \frac{p_{\gamma }}{c},
\end{equation}$$
where p γ is the photon momentum, E γ is the photon energy, and c is the speed of light in a vacuum.
According to Newton’s law of gravitation, the attraction force (
${\bm F}_{\rm G}$
) acting on a photon at the distance r from the lens, directed along the line connecting both objects, is represented as:
$$\begin{equation}
{\bm F}_{\rm G} = - \frac{G \, m_{\gamma } \, \mathfrak {M}}{r^3}\,{\bm r},
\end{equation}$$
where G = 6.674 ×10− 11 m3 kg− 1 s− 2 is the universal gravitational constant, r is the radius-vector of the photon, drawn from the centre of the lens, and r is its module.
We assume that the original photon was moving along a straight line with the impact parameter b (see Figure 2a). As a result of interaction with the lens, the photon will move along a geodesic curve, approaching the lens. The deflection angle (θ) of the photon γ is the angle between the initial and final momenta of photons (see Figure 2a). The deviation from the straight running depends on the body mass
$\mathfrak {M}$
and the impact parameter b.
The scattering of a photon in the gravitational field of a lens.
We consider the case of weak gravitational fields for a spherical body when the curvature of the trajectory of a photon can be neglected in the calculations; in other words, we assume that the photon moves in a straight line AB (see Figure 2b) all the interaction time.
Using the law of change of momentum and the Cartesian coordinate system, which is shown in Figure 2b, we obtain the projections of the momentum change (relative to the initial direction of motion) in the form of
$$\begin{equation}
\left.\begin{array}{l}\displaystyle \Delta p_{\parallel } = - \frac{G \, m_{\gamma } \, \mathfrak {M}}{c} \! \int _{-\infty }^{+\infty }\!\!\!\! \frac{x\, dx}{(x^2+b^2)^{\frac{3}{2}}}, \\
[4mm] \displaystyle \Delta p_{\perp } = - \frac{G \, m_{\gamma } \, \mathfrak {M}\, b}{c} \! \int _{-\infty }^{+\infty }\!\!\!\! \frac{dx}{(x^2+b^2)^{\frac{3}{2}}}. \end{array}\right\rbrace
\end{equation}$$
Obviously, the first integral of the system (22) is zero (Vygodsky Reference Vygodsky2006).
Performing a series of mathematical transformations, we obtain for the second integral the following result:
$$\begin{equation*}
\Delta p_{\perp } = - \frac{2 G \, m_{\gamma } \, \mathfrak {M}}{b\,c} = - \frac{2 G \, p_{\gamma }^{\mathrm{(i)}} \, \mathfrak {M}}{b\,c^2}.
\end{equation*}$$
The result is obtained in the Newtonian approximation—potential theory of gravitation. However, Albert Einstein predicted that the exact gravitational theory must be tensor theory, and the curvature of space gives as large contribution to the final result in Δp ⊥ as Newton’s theory of gravitation, according to Landau & Lifshitz (Reference Landau and Lifshitz2003). Hence, we write the following expression for the momentum change:
$$\begin{equation}
\Delta p_{\perp } = - \frac{4 G \, p_{\gamma }^{\mathrm{(i)}} \, \mathfrak {M}}{b\,c^2},\,\,\, \tan \theta = \frac{|\Delta p_{\perp }|}{p_{\gamma }^{\mathrm{(i)}}} = \frac{4 G \, \mathfrak {M}}{b\,c^2}.
\end{equation}$$
Since the angle θ is small, in practice it is customarily measured in arcsec:
$$\begin{equation}
\theta ^{\prime \prime }\, = \frac{4 G \, \mathfrak {M}}{b\,c^2} \times 206265^{\prime \prime }\, = \frac{2\,\mathfrak {R}_{{\rm Sh}}}{b} \times \ 206265^{\prime \prime }\,,
\end{equation}$$
where
$\mathfrak {R}_{\mathrm{Sh}}$
is the Schwarzschild radius for a lens, which is defined by the expression:
$$\begin{equation}
\mathfrak {R}_{\mathrm{Sh}} = \frac{2 G \, \mathfrak {M}}{c^2}.
\end{equation}$$
Using (1) and (6), we obtain the following ranges of possible values for
$\mathfrak {R}_{\mathrm{Sh}}$
(in
$\mathfrak {R}_J$
) for Nemesis, Tyche, P9, and a trans-Plutonian planet, other than P9:
$$\begin{equation}
\left.\begin{array}{l}\displaystyle 5.120 \times \ 10^{-7} \le \frac{\mathfrak {R}_{\mathrm{Sh}}^{N}}{{R}_{\mathrm{J}}} \le 2.888 \times \ 10^{-6}, \\
[4mm] \displaystyle 3.939 \times \ 10^{-8} \le \frac{\mathfrak {R}_{\mathrm{Sh}}^{T}}{{R}_{\mathrm{J}}} \le 5.120 \times \ 10^{-7}, \\
[4mm] \displaystyle 1.389 \times \ 10^{-8} \le \frac{\mathfrak {R}_{\mathrm{Sh}}^{P9}}{{R}_{\oplus }} \le 2.083 \times \ 10^{-8}, \\
[4mm] \displaystyle 1.389 \times \ 10^{-9} \le \frac{\mathfrak {R}_{\mathrm{Sh}}^{TP}}{{R}_{\oplus }} \le 2.083 \times \ 10^{-8}. \end{array}\right\rbrace
\end{equation}$$
The angle θ arcsec, according to (24), does not depend on photon frequency (wavelength). This property is called the achromatic effect of the lensing.
Figure 3a illustrates the deflection angle θ arcsec dependence on Nemesis’ mass (within the range 13 to 73 M
J) for the impact parameter b = 1.5 ×R
J. This dependence is linear with the angle and varies within the range 0.14 − 0.80 arcsec. In the case of Tyche (see Figure 4a), when the mass of the planet varies within the range of 1 to 13 M
J, the angle θ arcsec has the values 0.012 − 0.140 arcsec. Figures 5a, 6a show the regions of possible values of the deflection angle θ arcsec as a function of the mass for P9 and a trans-Plutonian planet, other than P9, respectively. Any theoretical dependencies on
$\mathfrak {M}_{P9}(\mathfrak {R}_{P9})$
,
$\mathfrak {M}_{TP}(\mathfrak {R}_{TP})$
, have not been taken into account because they are defined by the unknown internal structure of the hypothetical planet. It is obvious that the order of the deflection angle value is
${\cal O}(\mbox{1 mas})$
.
The curves of the deflection angle of the light beam in the gravitational field of Nemesis depending on (a) Nemesis’ mass (expressed in Jupiter masses, M J), where b = 1.5 ×R J; (b) the impact parameter b (expressed in Jupiter radii, R J).
The curves of the deflection angle of the light beam in the gravitational field of Tyche depending on (a) Tyche’s mass (expressed in Jupiter masses, M J), where b = 1.5 ×R J; (b) the impact parameter b (expressed in Jupiter radii, R J).
The curves of the deflection angle of the light beam in the gravitational field of Planet Nine depending on (a) its mass (expressed in Earth masses, M ⊕), for two boundary values of its radius (2R ⊕ and 4R ⊕); (b) the impact parameter b (expressed in Earth radii, R ⊕).
The curves of the deflection angle of the light beam in the gravitational field of trans-Plutonian planet depending on (a) its mass (expressed in Earth masses, M ⊕), for two boundary values of its radius (R ⊕ and 4R ⊕); (b) the impact parameter b (expressed in Earth radii, R ⊕).
In Figures 3b–6b, the curves of the deflection angle θ arcsec dependence on the impact parameter b (expressed in R
J and R
⊕) in the cases of Nemesis, Tyche, P9, and a trans-Plutonian planet, different from P9, are shown. There are three curves for the case of Nemesis corresponding to three different values of the mass
$\mathfrak {M}_{\mathrm{N}} =\lbrace 13,45,73.3\rbrace {M}_{\mathrm{J}}$
(low-mass brown dwarf, intermediate-mass brown dwarf, and massive brown dwarf, respectively). In the case of Tyche, there are four curves corresponding to values of the mass
$\mathfrak {M}_{\mathrm{T}} =\lbrace 1,4,7,13\rbrace {M}_{\mathrm{J}}$
(Jupiter-like planet, intermediate-mass jovian planet, massive jovian planet, very massive jovian planet). In the case of P9, three curves are shown. They correspond to three different values of the mass
$\mathfrak {M}_{\mathrm{P9}} =\lbrace 10,12.5,15\rbrace {M}_{\mathrm{\oplus }}$
(massive Super-Earth with
$\mathfrak {R}_{\mathrm{P9}}=2R_{\oplus }$
, mega-Earth or mini-Neptune with
$\mathfrak {R}_{\mathrm{P9}}=3\,R_{\oplus }$
, and Neptune-like planet with
$\mathfrak {R}_{\mathrm{P9}}=4\,R_{\oplus }$
). In the case of a trans-Plutonian planet, other than P9, four curves are shown. They correspond to four different values of the mass
$\mathfrak {M}_{\mathrm{TP}} =\lbrace 1,5,10,15\rbrace {M}_{\mathrm{\oplus }}$
(Earth-like planet with
$\mathfrak {R}_{\mathrm{TP}}=R_{\oplus }$
, intermediate-mass Super-Earth with
$\mathfrak {R}_{\mathrm{TP}}=1.5\,R_{\oplus }$
, massive Super-Earth with
$\mathfrak {R}_{\mathrm{TP}}=2\,R_{\oplus }$
, and Neptune-like planet with
$\mathfrak {R}_{\mathrm{TP}}=4\,R_{\oplus }$
).
It is obvious that the deflection angle dependence on the impact parameter is hyperbolic. For all shown cases of Nemesis and Tyche, the value of the deflection angle is not less than 0.01 arcsec. This value is slightly smaller than the angular resolution of the HST (βarcsec = 0.05 arcsec), of the order of the angular resolution of the JWST (James Webb Space Telescope), that is βarcsec = 0.018 arcsec, and significantly larger than the theoretical estimate (βarcsec = 0.003 arcsec) of the angular resolution of the future E-ELT (European Extremely Large Telescope) with diameter D E-ELT = 39 m (Cunningham et al. Reference Cunningham, Evans, Monnet, Le Louarn and Andersen2008). Hence, θ arcsec will be measurable experimentally in the near future. The situation is different for P9 and any other trans-Plutonian planet. For all shown cases of P9 and a trans-Plutonian planet, the value of the deflection angle is not bigger than 2.9 mas. It is lower than the angular resolution of E-ELT. Hence, in the cases of P9 and a trans-Plutonian planet, other than P9, θ arcsec will not be measurable experimentally in the near future.
4.2. Differential and total cross-sections of photon scattering in the gravitational field of the lens
Since the trajectory of a single photon is not experimentally detected, what is usually measured is the flux of scattered particles (F sca). It is the number of particles scattered by a lens in a certain direction per unit time. The total cross section of scattering σ is defined by
$$\begin{equation}
\sigma = \frac{F_{\mathrm{sca}}}{j_{0}},
\end{equation}$$
where j 0 is the flux density of particles (photons) that is the number of particles, moving in the direction of the target, passing through a unit area per unit time.
The elastic scattering process can be described by a differential cross-section of scattering which is equal to the ratio of the particle flux dF sca, scattered into the solid angle dΩ, to the flux density of incident particles j 0 and the solid angle dΩ:
$$\begin{equation}
\frac{{\rm d} \sigma }{{\rm d}\Omega } = \frac{{\rm d} F_{\mathrm{sca}}}{j_{0}\, {\rm d} \Omega }.
\end{equation}$$
Using equations (28) and (23), we can express the differential cross-section of photon scattering as
$$\begin{equation}
\left[\frac{{\rm d} \sigma }{{\rm d} \Omega }\right] = \left(\frac{4 G \, \mathfrak {M}}{c^2}\right)^2\frac{\cos \theta }{\sin ^4\theta }.
\end{equation}$$
The total cross-section of scattering is
$$\begin{eqnarray}
\sigma _{\mathrm{tot}} &=& \int _{\Omega } \!\! \left[\frac{{\rm d} \sigma }{{\rm d} \Omega }\right] {\rm d} \Omega = 2\pi \left(\frac{4 G \, \mathfrak {M}}{c^2}\right)^2 \int _{\theta _{\min }}^{\theta _{\max }} \frac{\cos \theta }{\sin ^3 \theta } d \theta \nonumber \\
&= &4\,\pi \, \mathfrak {R}_{\mathrm{Sh}}^2\left[\frac{1}{\sin ^2 \theta _{\min }} - \frac{1}{\sin ^2 \theta _{\max }}\right], \end{eqnarray}$$
where θmax is the maximum deflection angle, which can be achieved under these conditions. According to equation (23), the angle is maximal when the impact parameter b is minimal. Obviously, it can not be less than the lens radius
$\mathfrak {R}$
, i.e.,
$b\ge \mathfrak {R}$
, then
$$\begin{equation}
\theta _{\max } = \arctan \left[\frac{4 G \, \mathfrak {M}}{\mathfrak {R} \,c^2}\right] \approx \frac{4 G \, \mathfrak {M}}{\mathfrak {R} \,c^2} = 2\frac{\mathfrak {R}_{\rm Sh}}{\mathfrak {R}}.
\end{equation}$$
θmin is the minimum deflection angle that can be detected by a telescope. Assuming that telescopic observations are performed in the visible part of the spectrum, this angle should be limited by the angular resolution of the telescope (β arcsec). As β arcsec we will use the theoretical value of the resolution for the largest ground-based telescope, the E-ELT with a diameter D E-ELT = 39 m:
$$\begin{eqnarray}
\theta _{\min }^{\prime \prime } &=& \beta ^{\prime \prime } = \frac{120^{\prime \prime }}{D_{\mathrm{E-ELT}}} = 3.08\times 10^{-3}\,^{\prime \prime }, \Rightarrow \\
\theta _{\min } &=& 1.492 \times \ 10^{-8} \,. \nonumber
\end{eqnarray}$$
In the numerical analysis of the results, it is more convenient to use dimensionless quantities of the differential and the total cross-sections, which can be obtained from (29) and (30) dividing by the area of the geometric cross-section of the lens body
$S_{\rm G} = \pi \mathfrak {R}^2$
. The formulae for the differential cross-section and the total cross-section are
$$\begin{eqnarray}
S_{\Omega } = \frac{1}{S_{\rm G}}\left[\frac{{\rm d} \sigma }{{\rm d} \Omega }\right] = \frac{4}{\pi } x^2 \frac{\cos \theta }{\sin ^4\theta },\,\,\, \theta _{\min } \le \theta \le \theta _{\max },
\end{eqnarray}$$
$$\begin{eqnarray}
S_{\mathrm{\rm tot}} = \frac{\sigma _{\rm tot}}{S_{\rm G}} = 4 x^2 \left[\theta _{\min }^{-2} - \left(\frac{1}{2x}\right)^2\right], \,\,\, \,\,\,x = \frac{\mathfrak {R}_{\mathrm{Sh}}}{\mathfrak {R}}.
\end{eqnarray}$$
As for Nemesis and Tyche, the parameter x belongs to the interval of possible values given by inequality (26).
Figures 7a and 8a illustrate the differential cross-section, S Ω, dependence on scattering of electromagnetic radiation in the gravitational field of Nemesis (Figure 7a), for three values of its mass, and Tyche (Figure 8a), for four different values of its mass, represented by the scattering angle θ arcsec (logarithmic scale). It can be seen that this relationship is linear; it is a function of the mass of the putative star or planet. When the mass of the gravitational lens decreases, the range of possible values for x is narrowed.
Dependence in the case of Nemesis of (a) the differential cross-section S Ω of electromagnetic radiation scattering in the gravitational field of a lens (for three values of its mass) on the scattering angle θ arcsec, (b) total cross-section S tot dependence on the parameter x.
Dependence in the case of Tyche of (a) the differential cross-section S Ω of electromagnetic radiation scattering in the gravitational field of a lens (for four values of its mass) on the scattering angle θ arcsec, (b) total cross-section S tot dependence on the parameter x.
In Figures 7b and 8b, the curves of the total cross-section, S tot, dependence on the value of the parameter x for Nemesis and Tyche are shown (logarithmic scale). It is obvious that the desired relationship in this case corresponds to a continuous increase as x grows. As it has been shown in the previous section, the value θmax is less than θmin for P9 and any other trans-Plutonian planet, then the values of the differential and total cross-sections, as given by equations (33) and (34), remain largely unaffected by changes in the scattering angle. Thus, the total cross-section is negative.
4.3. Lensed images
Let us consider the problem of imaging the primary point source of light by a gravitational lens. Suppose that a point gravitational lens (deflector) is located at the point D, a light source (background star) is located at S, and an observer is located at O (see Figure 9). At large distances from the lens, the photons practically move along straight lines. Therefore, their trajectories can be approximated by two straight lines, broken near the body D (at the points A and B). The angle α between them shows how the photon was bent, after passing through the gravitational field of the body D.
The curvature of the rays; the formation of the images of the source (S) in the gravitational field of a lens (D).
The angle between the direction of the deflector and the true position of the source S is denoted by θ. Two rays of light (shown by two bold lines), passed on the opposite side of the gravitating body, will be deflected from the initial direction towards the body. If the light source S is far away from the body D, the rays converge at some distant point (Zakharov & Sazhin Reference Zakharov and Sazhin1998).
From Figure 9, with the simplest properties of a plane triangle for △AOS, it is seen that
$$\begin{equation}
\alpha & = & \beta _1 + \gamma _1, \\
\end{equation}$$
$$\begin{equation}
\theta _1 & = & \theta + \beta _1,
\end{equation}$$
For the △AOS, according to the law of sines, we have
$$\begin{equation*}
\frac{AO}{\sin \gamma _1} = \frac{SA}{\sin \beta _1}.
\end{equation*}$$
Since the angles β1, γ1 are small, sinβ1 ≈ β1, sinγ1 ≈ γ1. Let us also assume that the angle θ is small; so SA ≈ SD = D sd, AO ≈ DO = D d. As a consequence,
$$\begin{equation}
D_{\rm d} \,\beta _1 = D_{{\rm sd}}\, \gamma _1.
\end{equation}$$
From equalities (35), (36), taking into account that
$\alpha = 4G\, \mathfrak {M} /(b\,c^2)$
, we have
$$\begin{equation*}
\theta _1 = \theta + \alpha - \gamma _1 = \theta + \frac{2 \mathfrak {R}_{\mathrm{Sh}}}{b} - \gamma _1.
\end{equation*}$$
Then, from (37), we obtain γ1 = β1(D d/D sd). In the above expression, we take into account that β1 = θ1 − θ, according to (36). We also consider that the impact parameter is given by b ≈ DA ≈ D d ×θ1. As a result, we have
$$\begin{equation*}
\theta _1 = \theta + \frac{2 \mathfrak {R}_{\mathrm{Sh}}}{D_{\rm d}\,\theta _1} - (\theta _1 - \theta )\frac{D_{\rm d}}{D_{{\rm sd}}}.
\end{equation*}$$
The equation can be reduced to the quadratic equation in the variable θ1:
$$\begin{eqnarray}
\theta _1^2 - \theta \theta _1 - \theta _0^2=0, \,\,\,
\end{eqnarray}$$
$$\begin{eqnarray}
\theta ^2_0 = \left(\frac{2\,\mathfrak {R}_{\mathrm{Sh}}}{D_{{\rm d}}}\right)\frac{D_{{\rm sd}}}{(D_{{\rm sd}}+D_{{\rm d}})}. \end{eqnarray}$$
Where θ0 is the Einstein ring angular radius. The equation (38) is called the equation of the spherically symmetric point gravitational lens. It is conveniently expressed in terms of the source annual parallax (πs) and the deflector annual parallax (πd). Since D
sd = D
s − D
d and
$D_{\rm s} = \frac{1\,\mathrm{AU}}{\pi _{\rm s}^{\prime \prime }}206265^{\prime \prime }$
,
$D_d=\frac{1\,\mathrm{AU}}{\pi _{\rm d}^{\prime \prime }}206265^{\prime \prime }$
(where π″s, π″d are expressed in arcseconds), then
$$\begin{eqnarray*}
\theta ^2_0 = \frac{2 \mathfrak {R}_{\rm Sh\,\odot }\,\pi _{\rm d}^{\prime \prime }}{206265^{\prime \prime }\times 1 \,\mathrm{AU}}\left(1 - \frac{\pi _{\rm s}^{\prime \prime }}{\pi _{\rm d}^{\prime \prime }}\right)\left(\frac{\mathfrak {M}}{\mathrm{M}_{\odot }}\right), \nonumber
\end{eqnarray*}$$
where
$\mathfrak {R}_{\rm Sh\,\odot } = 2G\,\mathrm{M}_{\odot } c^{-2} = 2.95$
km is the Schwarzschild radius of the Sun. Expressing θ0 in arcseconds, we have
$$\begin{equation}
\theta _0^{\prime \prime } = 9.025^{\prime \prime } \times \ 10^{-2} \times \ \sqrt{\pi _{\rm d}^{\prime \prime } \left(1 - \frac{\pi _{\rm s}^{\prime \prime }}{\pi _{\rm d}^{\prime \prime }}\right) \left(\frac{\mathfrak {M}}{\mathrm{M}_{\odot }}\right)}.
\end{equation}$$
For the background stars (belonging to the Milky Way), with annual parallax π″s ~ 10− 3 − 10− 2″ , the above quantity (with π″s ≪ πd″) can be expressed as
$$\begin{equation*}
\theta _0^{\prime \prime } \approx 9.025^{\prime \prime } \times \ 10^{-2} \times \sqrt{\pi _{\rm d}^{\prime \prime }\left(\frac{\mathfrak {M}}{\mathrm{M}_{\odot }}\right)}.
\end{equation*}$$
It is clear that the equation (38) has two real roots corresponding to the two images of the source:
$$\begin{equation}
\left.\begin{array}{l}\theta _1^{(1)} = \frac{1}{2}\theta + \frac{1}{2}\sqrt{\theta ^2+ 4 \theta _0^2}, \\
[2mm] \theta _1^{(2)} = \frac{1}{2}\theta - \frac{1}{2}\sqrt{\theta ^2+ 4 \theta _0^2}{\bf .} \end{array}\right\rbrace
\end{equation}$$
Figure 10 shows the curves of both solutions of the equation (38), the value of Δθ = θ(1) 1 − θ1 (2) related to the angle θ, and the angular radius of the Einstein ring θ0. If the rapprochement of the source and the deflector is close (θ → 0), then there is a bright pronounced phenomenon of lensing. In this case, the angular distance between the deflector and the images tends to be equal to the angular radius of the Einstein ring (θ0) and the distance between the images tends to 2θ0. In fact, the images are moving on the Einstein ring.
θ(1)
1, |θ(2)
1|, Δθ = θ(1)
1 − θ1
(2), θ0 dependencies on the deflection angle θ, where
$\mathfrak {M}_N = 0.07\,\mathfrak {M}_{\odot }$
, D
d = 30 kAU (for a Jupiter-sized brown dwarf).
Two images are not always visible. When the root θ(2)
1 becomes smaller than the angular radius of the deflector
$\rho (\mathfrak {R})$
,
$$\begin{equation*}
\rho (\mathfrak {R}) > \theta _1^{(2)},\,\,\, \mbox{where} \,\,\, \rho (\mathfrak {R}) = \frac{\mathfrak {R}}{D_{\rm d}},
\end{equation*}$$
a ray of light eclipsed by the gravitational lens and the image I
2 becomes invisible to the observer. Hence, in this case, we can observe only one image which position does not coincide with the position of the source. Figures 11a, b show the curves of θ(min)
0 and θ(max)
0 depending on heliocentric distance of the lens D
d for Nemesis and Tyche. It is clear that in the case of Nemesis its angular radius at any possible heliocentric distances is significantly smaller than the radius θ0. This means that the images, corresponding to Nemesis, are always visible and can be detected experimentally. In the case of Tyche, in most of the range of acceptable values r
T, both images are visible only if the distance r
T > 6060 AU and Tyche’s mass
$\mathfrak {M}_{\rm T}>{M}_{\rm J}$
. The situation for the cases of P9 and a trans-Plutonian planet, other than P9, is different. For descriptive reasons, we have defined the parameter Δ = ρ − θ0, as the difference of planet angular radius and Einstein ring angular radius.
$\theta _0^{(\max )}=\theta _0(\mathfrak {M}_{{\rm N},\,{\rm T}}^{(\max )})$
,
$\theta _0^{(\min )}=\theta _0(\mathfrak {M}_{{\rm N},\,{\rm T}}^{(\min )})$
, ρ dependencies on heliocentric distance of the lens D
d in cases of Nemesis (a), Tyche (b). Dependence of Δ on heliocentric distance of the lens D
d for three types of planet in the case of Planet Nine (c) and for four types of planet in the case of a trans-Plutonian planet, other than Planet Nine (d), defined in subsection 4.1.
For the entire ranges of distances and for all types of planets, Δ > 0 (see Figure 11c, d). Therefore, in principle, strong gravitational lensing is impossible because at least one image is always eclipsed by the body, but the gravitational microlensing is possible. Figure 12 illustrates the results of the modeling of trajectories of the source S and the images I 1 and I 2 in the plane of the lens for two values of the impact parameter: (a) θp = 0.005 arcsec, (b) θp = 0.05 arcsec. The arrows indicate the direction of their movement. It is important to note that the source S, the images, and the deflector are always located on the same straight line in the plane. One of the images (I 2) separates from the lens and the other (I 1) from the source when it is close to its Einstein ring.
The trajectories of the source (S) and its images (I
1 and I
2), which were created by a gravitational lens (Nemesis with mass of
$\mathfrak {M}_{N}=0.07\,\mathfrak {M}_{\odot }$
and a corresponding distance of D
d = 30 kAU), in the cases of θp = 0.005 arcsec (a), θp = 0.05 arcsec (b). The directions of motion of the source and its images as indicated by the arrows.
5 CONCLUSIONS
In this paper, eight facts indirectly supporting the existence of a massive dark body at the Solar System periphery are reviewed. The basic physical properties and orbital characteristics of four different hypothetical candidates are considered. The solution of the problem of the deflection angle determined in the gravitational field of a spherical lens is given. The numerical analysis of the results obtained for the cases of Nemesis, Tyche, P9, and a trans-Plutonian planet, other than P9, are presented. It is shown that only in the cases of Nemesis and Tyche the value of the deflection angle will be measurable in the near future with the aid of the JWST and the E-ELT. Analytical results for the differential and total cross-sections of photon scattering in a weak gravitational field corresponding to a spherical lens are included in its dimensionless form. It is shown that the corresponding function of dimensionless differential cross section S Ω takes an extremely large value due to the very small deflection angles θ arcsec and a dependence of the type sin− 4θ. Given the problem of the formation of images by a gravitational lens, it is shown that, in general, for the cases of Nemesis and Tyche, two images can be detected experimentally. Only in the case of Tyche with a mass close to the mass of Jupiter at a distance of less than 6 060 AU from the Sun, Tyche could be resolved in one of the images. In the cases of P9 and any other trans-Plutonian planet, for the entire ranges of distances and for all types of planet strong gravitational lensing is impossible, in principle, but gravitational microlensing is possible. Photometry of gravitational lensing for the cases of Nemesis and Tyche and microlensing for the cases of P9 and a trans-Plutonian planet, other than P9, requires additional analyses out of the scope of the present work and will be covered in a forthcoming paper.
ACKNOWLEDGEMENTS
We thank the anonymous reviewers for careful reading of the paper. We appreciate all suggestions that significantly improved the manuscript.
