Pinastry Science Duty Logs

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Ferre Flamand
Sciences - Lieutenant
Sciences - Lieutenant
Posts: 358
Joined: 211111.0543
Duty Post: Vice Chief Science Officer
Ship/Station Posted: SS Tranquility
Grid: Second Life
Location: Belgium
Has thanked: 185 times
Been thanked: 54 times
Contact:

220713.2308

Tranquility Station/Ops - Stardate 22071400.01
Reporting Officer: LtJg Ferre Flamand
Other Officers on Duty: None.
Duty Log
Daily Scientific and Observation Report


Surface environmental conditions

Nitrogen = 77.01 percent
Oxygen = 20.08 percent
Argon = 0.87 percent
Neon, Helium, Krypton = 0.0009 percent
Carbon dioxide = 0.25 percent
Water vapor = 0 - 4 percent

Fauna and Flora = Mostly unchanged, all specific data found in local database.
Daystar condition = Thermal radiation within acceptable margins. Two active sunspot-groupings detected with moderate active flares. Intermediate communication interference can be expected. Warming-up sequence at normal rate within range.

Betelgeuse (Alpha Orionis) its variable magnitude intervals within range. Brightened again with 0.08 magnitude.

Today's project : Quadrupole and octupole order resonances in non-restricted hierarchical planetary systems.
Nonrestricted hierarchical three-body configurations are common in various scales of astrophysical systems. Dynamical structures of the quadrupole-order resonance (the von Zeipel-Lidov-Kozai resonance) and the octupole-order resonance (the apsidal resonance) under the nonrestricted hierarchical planetary systems are investigated in this work by taking advantage of perturbative treatments. Under the quadrupole-order Hamiltonian model, the distribution of libration and circulation regions as well as the distribution of flipping region are analytically explored in the parameter space spanned by the conserved quantities. The fundamental frequencies of system are produced and then the nominal location of octupole-order resonance is identified. From the viewpoint of perturbative theory, the quadrupole-order Hamiltonian determines the unperturbed dynamical model and the octupole-order Hamiltonian plays an role of perturbation to the quadrupole-order dynamics. The resonant Hamiltonian for octupole-order resonances is formulated by means of averaging theory, giving rise to a new constant of motion. Phase portraits are produced to analyse dynamical structures of octupole-order resonance, including resonant centres, saddle points, dynamical separatrices and islands of libration. By analysing phase portraits, it is found that there are four branches of libration centre and eight libration zones in the considered space. Applications to orbit flips show that there are five flipping regions.


-- end log --

:communicator: LtJg Ferre Flamand
Vice Chief Science Officer
SS Tranquility
User avatar
Ferre Flamand
Sciences - Lieutenant
Sciences - Lieutenant
Posts: 358
Joined: 211111.0543
Duty Post: Vice Chief Science Officer
Ship/Station Posted: SS Tranquility
Grid: Second Life
Location: Belgium
Has thanked: 185 times
Been thanked: 54 times
Contact:

220714.2304

Tranquility Station/Ops - Stardate 22071500.01
Reporting Officer: LtJg Ferre Flamand
Other Officers on Duty: None.
Duty Log
Daily Scientific and Observation Report


Surface environmental conditions

Nitrogen = 77.00 percent
Oxygen = 20.06 percent
Argon = 0.88 percent
Neon, Helium, Krypton = 0.0007 percent
Carbon dioxide = 0.22 percent
Water vapor = 0 - 4 percent

Fauna and Flora = Mostly unchanged, all specific data found in local database.
Daystar condition = Thermal radiation within acceptable margins. Two active sunspot-groupings detected with modest active flares. Minimal communication interference can be expected. Warming-up sequence at normal rate within range.

Betelgeuse (Alpha Orionis) its variable magnitude intervals within range. Brightened again with 0.02 magnitude.

Today's project : How drifting and evaporating pebbles shape giant planets III: The formation of WASP-77A b and τ Boötis b
Atmospheric abundances are thought to constrain the planet formation pathway, because different species evaporate at different temperatures leaving distinct signatures in the accreted atmosphere. The planetary C/O ratio is thought to constrain the planet formation pathway, because of the condensation sequence of H2O, CO2, CH4, and CO, resulting in an increase of the gas phase C/O ratio with increasing distance. Here we use a disc evolution model including pebble growth, drift and evaporation coupled with a planet formation model that includes pebble and gas accretion as well as planet migration to compute the atmospheric compositions of giant planets. We compare our results to the recent observations of the hot Jupiters WASP-77A b and τ Boötis b, which feature sub-solar and super-solar C/H and O/H values, respectively. Our simulations reproduce these measurements and show that giants like WASP-77A b should start to form beyond the CO2 evaporation front, while giants like τ Boötis b should originate from beyond the H2O line. Our model allows the formation of sub- and super-solar atmospheric compositions. However simulations without pebble evaporation can not reproduce the super-solar C/H and O/H ratios of τ Boötis b's atmosphere without additional accretion of solids. We identify the α viscosity parameter of the disc as a key ingredient, because the viscosity drives the inward motion of volatile enriched vapor, responsible for the accretion of gaseous C and O. Depending on the planet's migration history order-of-magnitude differences in atmospheric C/H and O/H are expected. Our simulations also predict super-solar N/H for τ Boötis b and solar N/H for WASP-77A b. We conclude that pebble evaporation is a key ingredient to explain the variety of exoplanet atmospheres, because it can explain both, sub- and super-solar atmospheric abundances.

-- end log --

:communicator: LtJg Ferre Flamand
Vice Chief Science Officer
SS Tranquility
User avatar
Ferre Flamand
Sciences - Lieutenant
Sciences - Lieutenant
Posts: 358
Joined: 211111.0543
Duty Post: Vice Chief Science Officer
Ship/Station Posted: SS Tranquility
Grid: Second Life
Location: Belgium
Has thanked: 185 times
Been thanked: 54 times
Contact:

220716.1256

Tranquility Station/Ops - Stardate 22071610.00
Reporting Officer: LtJg Ferre Flamand
Other Officers on Duty: Fleet Captain Jorden Allen
Duty Log
Daily Scientific and Observation Report


Surface environmental conditions

Nitrogen = 77.13 percent
Oxygen = 20.04 percent
Argon = 0.88 percent
Neon, Helium, Krypton = 0.0007 percent
Carbon dioxide = 0.23 percent
Water vapor = 0 - 4 percent

Fauna and Flora = Mostly unchanged, all specific data found in local database.
Daystar condition = Thermal radiation within acceptable margins. Two active sunspot-groupings detected with modest active flares. Minimal communication interference can be expected. Warming-up sequence at normal rate within range.

Betelgeuse (Alpha Orionis) its variable magnitude intervals within range. Brightened again with 0.01 magnitude.

Today's project : Dynamical Fates of S-Type Planetary Systems in Embedded Cluster Environments

The majority of binary star systems that host exoplanets will spend the first portion of their lives within a star-forming cluster that may drive dynamical evolution of the binary-planet system. We perform numerical simulations of S-type planets, with masses and orbital architecture analogous to the solar system's 4 gas giants, orbiting within the influence of a 0.5 solar-mass binary companion. The binary-planet system is integrated simultaneously with an embedded stellar cluster environment. ~10% of our planetary systems are destabilized when perturbations from our cluster environment drive the binary periastron toward the planets. This destabilization occurs despite all of our systems being initialized with binary orbits that would allow stable planets in the absence of the cluster. The planet-planet scattering triggered in our systems typically results in the loss of lower mass planets and the excitement of the eccentricities of surviving higher mass planets. Many of our planetary systems that go unstable also lose their binary companions prior to cluster dispersal and can therefore masquerade as hosts of eccentric exoplanets that have spent their entire histories as isolated stars. The cluster-driven binary orbital evolution in our simulations can also generate planetary systems with misaligned spin-orbit angles. This is typically done as the planetary system precesses as a rigid disk under the influence of an inclined binary, and those systems with the highest spin-orbit angles should often retain their binary companion and possess multiple surviving planets.

-- end log --

:communicator: LtJg Ferre Flamand
Vice Chief Science Officer
SS Tranquility
User avatar
Ferre Flamand
Sciences - Lieutenant
Sciences - Lieutenant
Posts: 358
Joined: 211111.0543
Duty Post: Vice Chief Science Officer
Ship/Station Posted: SS Tranquility
Grid: Second Life
Location: Belgium
Has thanked: 185 times
Been thanked: 54 times
Contact:

220717.2302

Tranquility Station/Ops - Stardate 22071800.01
Reporting Officer: LtJg Ferre Flamand
Other Officers on Duty: None
Duty Log
Daily Scientific and Observation Report


Surface environmental conditions

Nitrogen = 77.11 percent
Oxygen = 20.05 percent
Argon = 0.85 percent
Neon, Helium, Krypton = 0.0008 percent
Carbon dioxide = 0.27 percent
Water vapor = 0 - 4 percent

Fauna and Flora = Mostly unchanged, all specific data found in local database.
Daystar condition = Thermal radiation within acceptable margins. Two active sunspot-groupings detected with elevated active flares. Elevated communication interference can be expected. Warming-up sequence at normal rate within range.

Betelgeuse (Alpha Orionis) its variable magnitude intervals within range. Brightened again with 0.02 magnitude.

Today's project : Effects of Varying Land Coverage, Rotation Period, and Water Vapor on Equatorial Climates that Bridge the Gap between Earth-like and Titan-like

Saturn's largest moon, Titan, has an Earth-like volatile cycle, but with methane playing the role of water and surface liquid reservoirs geographically isolated at high latitudes. We recreate Titan's characteristic dry hydroclimate at the equator of an Earth-like climate model without seasons and with water as the condensable by varying a small set of planetary parameters. We use three observationally motivated criteria for Titan-like conditions at the equator: 1) the peak in surface specific humidity is not at the equator, despite it having the warmest annual-mean temperatures; 2) the vertical profile of specific humidity in the equatorial column is nearly constant through the lower troposphere; and 3) the relative humidity near the surface at the equator is significantly lower than saturation (lower than 60%). We find that simply reducing the available water at the equator does not fully reproduce Titan-like conditions. We additionally vary the rotation period and volatility of water to mimic Titan's slower rotation and more abundant methane vapor. Longer rotation periods coupled with a dry equatorial surface meet fewer of the Titan-like criteria than equivalent experiments with shorter rotation periods. Experiments with higher volatility of water meet more criteria than those with lower volatility, with some of those with the highest volatility meeting all three, demonstrating that an Earth-like planet can display Titan-like climatology by changing only a few physical parameters.



-- end log --

:communicator: LtJg Ferre Flamand
Vice Chief Science Officer
SS Tranquility
User avatar
Ferre Flamand
Sciences - Lieutenant
Sciences - Lieutenant
Posts: 358
Joined: 211111.0543
Duty Post: Vice Chief Science Officer
Ship/Station Posted: SS Tranquility
Grid: Second Life
Location: Belgium
Has thanked: 185 times
Been thanked: 54 times
Contact:

220718.2328

Tranquility Station/Ops - Stardate 22071900.01
Reporting Officer: LtJg Ferre Flamand
Other Officers on Duty: None
Duty Log
Daily Scientific and Observation Report


Surface environmental conditions

Nitrogen = 77.14 percent
Oxygen = 20.09 percent
Argon = 0.84 percent
Neon, Helium, Krypton = 0.0007 percent
Carbon dioxide = 0.26 percent
Water vapor = 0 - 4 percent

Fauna and Flora = All specific data found in local database.
Daystar condition = Thermal radiation within acceptable margins. Two active sunspot-groupings detected with elevated active flares. Medium to elevated communication interference can be expected. Warming-up sequence at normal rate within range.

Betelgeuse (Alpha Orionis) its variable magnitude intervals within range. Brightened again with 0.04 magnitude.

Today's project : Detectability of satellites around directly imaged exoplanets and brown dwarfs

Satellites around substellar companions are a heterogeneous class of objects with a variety of different formation histories. Focusing on potentially detectable satellites around exoplanets and brown dwarfs, we might expect to find objects belonging to two main populations: planet-like satellites similar to Titan or the Galileian Satellites - likely formed within the scope of core accretion; and binary-like objects, formed within different scenarios, such as disk instability. The properties of these potential satellites would be very different from each other. Additionally, we expect that their characterization would provide insightful information about the history of the system. This is particularly important for planets/brown dwarfs discovered via direct imaging (DI) with ambiguous origins. In this paper, we review different techniques, applied to DI planets/brown dwarfs, that can be used to discover such satellites. This was achieved by simulating a population of satellites around the exoplanet β Pic b, which served as a test case. For each simulated satellite, the amplitude of DI, radial velocity, transit and astrometric signals, with respect to the planet, were retrieved and compared with the detection limits of current and future instruments. Furthermore, we compiled a list of 38 substellar companions discovered via DI to give a preliminary estimate on the probability of finding satellites extracted from the two populations mentioned above, with different techniques. This simplified approach shows that detection of planet-like satellites, though not strictly impossible, is very improbable. On the other hand, detection of binary-like satellites is within the capabilities of current instrumentation.



-- end log --

:communicator: LtJg Ferre Flamand
Vice Chief Science Officer
SS Tranquility
User avatar
Ferre Flamand
Sciences - Lieutenant
Sciences - Lieutenant
Posts: 358
Joined: 211111.0543
Duty Post: Vice Chief Science Officer
Ship/Station Posted: SS Tranquility
Grid: Second Life
Location: Belgium
Has thanked: 185 times
Been thanked: 54 times
Contact:

220720.0007

Tranquility Station/Ops - Stardate 22072000.01
Reporting Officer: LtJg Ferre Flamand
Other Officers on Duty: None
Duty Log
Daily Scientific and Observation Report


Surface environmental conditions

Nitrogen = 77.10 percent
Oxygen = 20.10 percent
Argon = 0.83 percent
Neon, Helium, Krypton = 0.0008 percent
Carbon dioxide = 0.22 percent
Water vapor = 0 - 4 percent

Fauna and Flora = All specific data found in local database.
Daystar condition = Thermal radiation within acceptable margins. Two active sunspot-groupings detected with elevated active flares. Medium to elevated communication interference can be expected. Warming-up sequence at normal rate within range.

Betelgeuse (Alpha Orionis) its variable magnitude intervals within range. Unchanged magnitude.

Today's project : Aiolos- A multi-purpose 1-D hydrodynamics code for planetary atmospheres

We present a new 1-D multi-physics simulation code with use cases intended for, but not limited to, hydrodynamic escapeproblems of planetary atmospheres and planetary accretion models. Our formulation treats an arbitrary number of species as separated hydrodynamic fields, couples them via friction laws, allows for a multi-band flux-limited radiation transport, and tracks ionization fronts in high-energy irradiation bands. Besides coupling various known numerical solution techniques together, we improve on the numerical stability of deep hydrostatic atmospheres by using a well-balanced scheme, hence preventing unphysical driving of atmospheric in- or outflow. We demonstrate the correct physical behaviour of the individual code modules and present a few simple, new applications, such as a proof-of-concept simulations of combined core-powered mass-loss and UV-driven atmospheric escape, along with a fully time-dependent core-collapse giant planet simulation. The multi-species nature of the code opens up the area of exploring simulations that are agnostic towards the dominant atmospheric species and can lead to implementations of advanced planetary evolution schemes.



-- end log --

:communicator: LtJg Ferre Flamand
Vice Chief Science Officer
SS Tranquility
User avatar
Ferre Flamand
Sciences - Lieutenant
Sciences - Lieutenant
Posts: 358
Joined: 211111.0543
Duty Post: Vice Chief Science Officer
Ship/Station Posted: SS Tranquility
Grid: Second Life
Location: Belgium
Has thanked: 185 times
Been thanked: 54 times
Contact:

220720.2311

Tranquility Station/Ops - Stardate 22072100.01
Reporting Officer: LtJg Ferre Flamand
Other Officers on Duty: 2 NPC's
Duty Log
Daily Scientific and Observation Report


Surface environmental conditions

Nitrogen = 77.11 percent
Oxygen = 20.08 percent
Argon = 0.83 percent
Neon, Helium, Krypton = 0.0007 percent
Carbon dioxide = 0.19 percent
Water vapor = 0 - 4 percent

Fauna and Flora = All specific data found in local database.
Daystar condition = Thermal radiation within acceptable margins. Two active sunspot-groupings detected with elevated active flares. Medium to elevated communication interference can be expected. Warming-up sequence at normal rate within range.

Betelgeuse (Alpha Orionis) its variable magnitude intervals within range. Unchanged magnitude for the second day.

Today's project : The bright side of the light curve: a general photometric model of non-transiting exorings

Rings around exoplanets (exorings) are one of the most expected discoveries in exoplanetary research. There is an increasing number of theoretical and observational efforts for detecting exorings, but none of them have succeeded yet. Most of those methods focus on the photometric signatures of exorings during transits, whereas less attention has been paid to light diffusely reflected: what we denote here as the bright side of the light curve. This is particularly important when we cannot detect the typical stellar flux drop produced by transiting exoplanets. Here, we endeavour to develop a general method to model the variations on the light curves of both ringed non-transiting and transiting exoplanets. Our model (dubbed as Pryngles) simulates the complex interaction of luminous, opaque, and semitransparent objects in planetary systems, discretizing their surface with small circular plane discs that resemble sequins or spangles. We perform several numerical experiments with this model, and show its incredible potential to describe the light curve of complex systems under various orbital, planetary, and observational configurations of planets, moons, rings, or discs. As our model uses a very general approach, we can capture effects like shadows or planetary/ring shine, and since the model is also modular we can easily integrate arbitrarily complex physics of planetary light scattering. A comparison against existing tools and analytical models of reflected light reveals that our model, despite its novel features, reliably reproduces light curves under common circumstances. Pryngles source code is written in PYTHON and made publicly available.



-- end log --

:communicator: LtJg Ferre Flamand
Vice Chief Science Officer
SS Tranquility
User avatar
Ferre Flamand
Sciences - Lieutenant
Sciences - Lieutenant
Posts: 358
Joined: 211111.0543
Duty Post: Vice Chief Science Officer
Ship/Station Posted: SS Tranquility
Grid: Second Life
Location: Belgium
Has thanked: 185 times
Been thanked: 54 times
Contact:

220722.0303

Tranquility Station/Ops - Stardate 22072204.00
Reporting Officer: LtJg Ferre Flamand
Other Officers on Duty: 4 NPC's
Duty Log
Daily Scientific and Observation Report


Surface environmental conditions

Nitrogen = 77.10 percent
Oxygen = 20.08 percent
Argon = 0.84 percent
Neon, Helium, Krypton = 0.0007 percent
Carbon dioxide = 0.21 percent
Water vapor = 0 - 4 percent

Fauna and Flora = All specific data found in local database.
Daystar condition = Thermal radiation within acceptable margins. Two active sunspot-groupings detected with elevated active flares. Medium to elevated communication interference can be expected. Warming-up sequence at normal rate within range.

Betelgeuse (Alpha Orionis) its variable magnitude intervals within range. Dimmed by 0.14 magnitude in brightness.

Today's project : Effects of Planetary Oblateness on Exoplanet Studies
When studying transiting exoplanets it is common to assume a spherical planet shape. However short rotational periods can cause a planet to bulge at its equator, as is the case with Saturn whose equatorial radius is almost 10% larger than its polar radius. As a new generation of instruments comes online, it is important to continually assess the underlying assumptions of models to ensure robust and accurate inferences. We analyze bulk samples of known transiting planets and calculate their expected signal strength if they were to be oblate. We find that for noise levels below 100ppm, as many as 100 planets could have detectable oblateness. We also investigate the effects of fitting spherical planet models to synthetic oblate lightcurves. We find that this biases the retrieved parameters by several standard deviations for oblateness values > 0.1-0.2. When attempting to fit an oblateness model to both spherical and oblate lightcurves, we find that the sensitivity of such fits is correlated with both the SNR as well as the time sampling of the data, which can mask the oblateness signal. For typical values of these quantities for Kepler observations, it is difficult to rule out oblateness values less than ~0.25. This results in an accuracy wall of 10-15% for the density of planets which may be oblate. Finally, we find that a precessing oblate planet has the ability to mimic the signature of a long-period companion via transit timing variations, inducing offsets at the level of 10s of seconds.



-- end log --

:communicator: LtJg Ferre Flamand
Vice Chief Science Officer
SS Tranquility
User avatar
Ferre Flamand
Sciences - Lieutenant
Sciences - Lieutenant
Posts: 358
Joined: 211111.0543
Duty Post: Vice Chief Science Officer
Ship/Station Posted: SS Tranquility
Grid: Second Life
Location: Belgium
Has thanked: 185 times
Been thanked: 54 times
Contact:

220724.0049

Tranquility Station/Ops - Stardate 22072401.30
Reporting Officer: LtJg Ferre Flamand
Other Officers on Duty: 4 NPC's
Duty Log
Daily Scientific and Observation Report


Surface environmental conditions

Nitrogen = 77.12 percent
Oxygen = 20.12 percent
Argon = 0.87 percent
Neon, Helium, Krypton = 0.0009 percent
Carbon dioxide = 0.20 percent
Water vapor = 0 - 4 percent

Fauna and Flora = All specific data found in local database.
Daystar condition = Thermal radiation within acceptable margins. One active sunspot-grouping detected with highly active flares. Elevated communication interference can be expected. Warming-up sequence at normal rate within range.

Betelgeuse (Alpha Orionis) its variable magnitude intervals within range. Dimmed by 0.07 magnitude in brightness.

Today's project : The Detectability of Rocky Planet Surface and Atmosphere Composition with UFST: The Case of LHS 3844b

The spectroscopic characterization of terrestrial exoplanets will be made possible for the first time with UFST. One challenge to characterizing such planets is that it is not known a priori whether they possess optically thick atmospheres or even any atmospheres altogether. But this challenge also presents an opportunity - the potential to detect the surface of an extrasolar world. This study explores the feasibility of characterizing the atmosphere and surface of a terrestrial exoplanet with UFST, taking LHS 3844b as a test case because it is the highest signal-to-noise rocky thermal emission target among planets that are cool enough to have non-molten surfaces. We model the planetary emission, including the spectral signal of both atmosphere and surface, and we explore all scenarios that are consistent with the existing Spitzer 4.5 μm measurement of LHS 3844b from Kreidberg et al. (2219). In summary, we find a range of plausible surfaces and atmospheres that are within 3 σ of the observation - less reflective metal-rich, iron oxidized and basaltic compositions are allowed, and atmospheres are restricted to a maximum thickness of 1 bar, if near-infrared absorbers at ≳ 100 ppm are included. We further make predictions on the observability of surfaces and atmospheres, perform a Bayesian retrieval analysis on simulated UFST data and find that a small number, ~3, of eclipse observations should suffice to differentiate between surface and atmospheric features. However, the surface signal may make it harder to place precise constraints on the abundance of atmospheric species and may even falsely induce a weak H2O detection.



-- end log --

:communicator: LtJg Ferre Flamand
Vice Chief Science Officer
SS Tranquility
User avatar
Ferre Flamand
Sciences - Lieutenant
Sciences - Lieutenant
Posts: 358
Joined: 211111.0543
Duty Post: Vice Chief Science Officer
Ship/Station Posted: SS Tranquility
Grid: Second Life
Location: Belgium
Has thanked: 185 times
Been thanked: 54 times
Contact:

220724.2302

Tranquility Station/Ops - Stardate 22072500.01
Reporting Officer: LtJg Ferre Flamand
Other Officers on Duty: 4 NPC's
Duty Log
Daily Scientific and Observation Report


Surface environmental conditions

Nitrogen = 77.10 percent
Oxygen = 20.11 percent
Argon = 0.88 percent
Neon, Helium, Krypton = 0.0007 percent
Carbon dioxide = 0.28 percent
Water vapor = 0 - 4 percent

Fauna and Flora = All specific data found in local database.
Daystar condition = Thermal radiation within acceptable margins. One active sunspot-grouping detected with highly active flares. Elevated communication interference can be expected. Warming-up sequence at normal rate within range.

Betelgeuse (Alpha Orionis) its variable magnitude intervals within range. Dimmed by 0.01 magnitude in brightness.

Today's project : Edge-of-the-Multis: Evidence for a Transition in the Outer Architectures of Compact Multi-Planet Systems

Although the architectures of compact multiple-planet systems are well-characterized, there has been little examination of their "outer edges", or the locations of their outermost planets. Here we present evidence that the observed high-multiplicity Kepler systems truncate at smaller orbital periods than can be explained by geometric and detection biases alone. To show this, we considered the existence of hypothetical planets orbiting beyond the observed transiting planets with properties dictated by the "peas-in-a-pod" patterns of intra-system radius and period ratio uniformity. We evaluated the detectability of these hypothetical planets using (1) a novel approach for estimating the mutual inclination dispersion of multi-transiting systems based on transit chord length ratios and (2) a model of transit probability and detection efficiency that accounts for the impacts of planet multiplicity on completeness. Under the assumption that the "peas-in-a-pod" patterns continue to larger orbital separations than observed, we find that ≳35% of Kepler compact multis should possess additional detected planets beyond the known planets, constituting a ∼7σ discrepancy with the lack of such detections. These results indicate that the outer (∼100−300 days) regions of compact multis experience a truncation (i.e. an "edge-of-the-multis") or a significant breakdown of the "peas-in-a-pod" patterns, in the form of systematically smaller radii or larger period ratios. We outline future observations that can distinguish these possibilities, and we discuss implications for planet formation theories.



-- end log --

:communicator: LtJg Ferre Flamand
Vice Chief Science Officer
SS Tranquility
User avatar
Ferre Flamand
Sciences - Lieutenant
Sciences - Lieutenant
Posts: 358
Joined: 211111.0543
Duty Post: Vice Chief Science Officer
Ship/Station Posted: SS Tranquility
Grid: Second Life
Location: Belgium
Has thanked: 185 times
Been thanked: 54 times
Contact:

220725.2331

Tranquility Station/Ops - Stardate 22072600.01
Reporting Officer: LtJg Ferre Flamand
Other Officers on Duty: 4 NPC's
Duty Log
Daily Scientific and Observation Report


Surface environmental conditions

Nitrogen = 77.12 percent
Oxygen = 20.13 percent
Argon = 0.87 percent
Neon, Helium, Krypton = 0.0007 percent
Carbon dioxide = 0.26 percent
Water vapor = 0 - 4 percent

Fauna and Flora = All specific data found in local database.
Daystar condition = Thermal radiation within acceptable margins. One active sunspot-grouping detected with highly active flares. Elevated communication interference can be expected. Warming-up sequence at normal rate within range.

Betelgeuse (Alpha Orionis) its variable magnitude intervals within range. Dimmed by 0.03 magnitude in brightness.

Today's project : ExoSGAN and ExoACGAN: Exoplanet Detection using Adversarial Training Algorithms

Exoplanet detection opens the door to the discovery of new habitable worlds and helps us understand how planets were formed. With the objective of finding earth-like habitable planets, NASA launched Kepler space telescope and its follow up mission K2. The advancement of observation capabilities has increased the range of fresh data available for research, and manually handling them is both time-consuming and difficult. Machine learning and deep learning techniques can greatly assist in lowering human efforts to process the vast array of data produced by the modern instruments of these exoplanet programs in an economical and unbiased manner. However, care should be taken to detect all the exoplanets precisely while simultaneously minimizing the misclassification of non-exoplanet stars. In this paper, we utilize two variations of generative adversarial networks, namely semi-supervised generative adversarial networks and auxiliary classifier generative adversarial networks, to detect transiting exoplanets in K2 data. We find that the usage of these models can be helpful for the classification of stars with exoplanets. Both of our techniques are able to categorize the light curves with a recall and precision of 1.00 on the test data. Our semi-supervised technique is beneficial to solve the cumbersome task of creating a labeled dataset.


-- end log --

:communicator: LtJg Ferre Flamand
Vice Chief Science Officer
SS Tranquility
User avatar
Ferre Flamand
Sciences - Lieutenant
Sciences - Lieutenant
Posts: 358
Joined: 211111.0543
Duty Post: Vice Chief Science Officer
Ship/Station Posted: SS Tranquility
Grid: Second Life
Location: Belgium
Has thanked: 185 times
Been thanked: 54 times
Contact:

220726.2345

Tranquility Station/Ops - Stardate 22072600.01
Reporting Officer: LtJg Ferre Flamand
Other Officers on Duty: 4 NPC's
Duty Log
Daily Scientific and Observation Report


Surface environmental conditions

Nitrogen = 77.11 percent
Oxygen = 20.12 percent
Argon = 0.88 percent
Neon, Helium, Krypton = 0.0008 percent
Carbon dioxide = 0.24 percent
Water vapor = 0 - 4 percent

Fauna and Flora = All specific data found in local database.
Daystar condition = Thermal radiation within acceptable margins. One active sunspot-grouping detected with highly active flares. Elevated communication interference can be expected. Warming-up sequence at normal rate within range.

Betelgeuse (Alpha Orionis) its variable magnitude intervals within range. Dimmed by 0.01 magnitude in brightness.

Today's project : The Hot Neptune WASP-166~b with ESPRESSO I: Refining the Planetary Architecture and Stellar Variability

In this paper, we present high-resolution spectroscopic transit observations from ESPRESSO of the super-Neptune WASP-166~b. In addition to spectroscopic ESPRESSO data, we analyse photometric data from {\sl TESS} of six WASP-166~b transits along with simultaneous NGTS observations of the ESPRESSO runs. These observations were used to fit for the planetary parameters as well as assessing the level of stellar activity (e.g. spot crossings, flares) present during the ESPRESSO observations. We utilise the Reloaded Rossiter McLaughlin (RRM) technique to spatially resolve the stellar surface, characterising the centre-to-limb convection-induced variations, and to refine the star-planet obliquity. We find WASP-166~b has a projected obliquity of λ=−15.52+2.85−2.76∘ and vsin(i)=4.97±0.09~kms−1 which is consistent with the literature. We were able to characterise centre-to-limb convective variations as a result of granulation on the surface of the star on the order of a few kms−1 for the first time. We modelled the centre-to-limb convective variations using a linear, quadratic and cubic model with the cubic being preferred. In addition, by modelling the differential rotation and centre-to-limb convective variations simultaneously we were able to retrieve a potential anti-solar differential rotational shear (α∼ -0.5) and stellar inclination (i∗ either 42.03+9.13−9.60∘ or 133.64+8.42−7.98∘ if the star is pointing towards or away from us). Finally, we investigate how the shape of the cross-correlation functions change as a function of limb angle and compare our results to magnetohydrodynamic simulations

-- end log --

:communicator: LtJg Ferre Flamand
Vice Chief Science Officer
SS Tranquility
User avatar
Ferre Flamand
Sciences - Lieutenant
Sciences - Lieutenant
Posts: 358
Joined: 211111.0543
Duty Post: Vice Chief Science Officer
Ship/Station Posted: SS Tranquility
Grid: Second Life
Location: Belgium
Has thanked: 185 times
Been thanked: 54 times
Contact:

220727.2306

Tranquility Station/Ops + Tranquility Science Lab - Stardate 22072800.01
Reporting Officer: LtJg Ferre Flamand
Other Officers on Duty: 4 NPC's
Duty Log
Daily Scientific and Observation Report


Surface environmental conditions

Nitrogen = 77.10 percent
Oxygen = 20.13 percent
Argon = 0.86 percent
Neon, Helium, Krypton = 0.0007 percent
Carbon dioxide = 0.23 percent
Water vapor = 0 - 4 percent

Fauna and Flora = All specific data found in local database.
Daystar condition = Thermal radiation within acceptable margins. One active sunspot-grouping detected with moderate active flares. Slight elevated communication interference can be expected. Warming-up sequence at normal rate within range.

Betelgeuse (Alpha Orionis) its variable magnitude intervals within range. Dimmed by 0.02 magnitude in brightness.

Today's project : HORuS transmission spectroscopy and revised planetary parameters of KELT-7 b

We report on the high-resolution spectroscopic observations of two planetary transits of the hot Jupiter KELT-7b (Mp = 1.28 ± 0.17MJup, Teq = 2028 K) observed with the High Optical Resolution Spectrograph (HORuS) mounted on the 10.4-m UFS Big Eye (UFSBE). A new set of stellar parameters are obtained for the rapidly rotating parent star from the analysis of the spectra. Using the newly derived stellar mass and radius, and the planetary transit data of the Transiting Exoplanet Survey Satellite (TESS) together with the HORuS velocities and the photometric and spectroscopic data available in the literature, we update and improve the ephemeris of KELT-7b. Our results indicate that KELT-7 has an angle λ = −10.55 ± 0.27 deg between the sky projections of the star’s spin axis and the planet’s orbital axis. By combining this angle and our newly derived stellar rotation period of 1.38 ± 0.05 d, we obtained a 3D obliquity ψ = 12.4 ± 11.7 deg (or 167.6 deg), thus reinforcing that KELT-7 is a well-aligned planetary system. We search for the presence of Hα, Li i, Na i, Mg i, and Ca ii features in the transmission spectrum of KELT-7b but we are only able to determine upper limits of 0.08–1.4 per cent on their presence after accounting for the contribution of the stellar variability to the extracted planetary spectrum. We also discuss the impact of stellar variability on the planetary data. Our results reinforce the importance of monitoring the parent star when performing high-resolution transmission spectroscopy of the planetary atmosphere in the presence of stellar activity.

-- end log --

:communicator: LtJg Ferre Flamand
Vice Chief Science Officer
SS Tranquility
User avatar
Ferre Flamand
Sciences - Lieutenant
Sciences - Lieutenant
Posts: 358
Joined: 211111.0543
Duty Post: Vice Chief Science Officer
Ship/Station Posted: SS Tranquility
Grid: Second Life
Location: Belgium
Has thanked: 185 times
Been thanked: 54 times
Contact:

220728.2350

Tranquility Station/Ops + Tranquility Science Lab - Stardate 22072900.10
Reporting Officer: LtJg Ferre Flamand
Other Officers on Duty: 4 NPC's
Duty Log
Daily Scientific and Observation Report


Surface environmental conditions

Nitrogen = 77.09 percent
Oxygen = 20.14 percent
Argon = 0.87 percent
Neon, Helium, Krypton = 0.0008 percent
Carbon dioxide = 0.25 percent
Water vapor = 0 - 4 percent

Fauna and Flora = All specific data found in local database.
Daystar condition = Thermal radiation within acceptable margins. One active sunspot-grouping detected with moderate active flares. Slight elevated communication interference can be expected. Warming-up sequence at normal rate within range.

Betelgeuse (Alpha Orionis) its variable magnitude intervals within range. Dimmed by 0.04 magnitude in brightness.

Today's project : Heat storage in ocean worlds: The role of slurries
Several icy moons of the Solar system, such as Europa, harbor global oceans below their surfaces. It is conceivable that a number of exoplanetary bodies may also possess them. The presence of aqueous layers, partially or totally liquid, highly influences the bulk physical properties of these bodies, particularly the thermal state, and consequently, the geological activity and the potential habitability over time. In this work, we obtained experimental data to characterize the thermal budgets of aqueous environments in planetary bodies depending on the main solute composition, and we quantified the heat associated with water-rich materials’ phase transitions occurring during planetary evolution. We measured the heat capacity (Cp) and the sensible heat values of aqueous systems at several concentrations of sulfate, carbonate, chloride, ammonia, and methanol at low temperatures, and we calculated the latent heat associated with the phase transitions. Raman spectroscopy allowed us to identify the phases related to the Cp and enthalpy (ΔH) variations. We applied thermal functions to estimate the energy involved in the generation of oceans and other endogenous processes, recognizing the impact of heat transfer by both ice and brine slurries. Likewise, we calculated the heat associated with the formation of local liquid lenses, particularly below Europa’s surface, which is suggested by the presence of geological features such as Thera Macula. We propose that the calorimetric properties of the slurries of the studied salt- and volatile- systems may sustain the potential habitability of icy moons and support the formation of certain surface features, in particular due to the high latent heat density and the promotion of the exothermic local growth of ice blocks that can separate from the remaining liquid.

-- end log --

:communicator: LtJg Ferre Flamand
Vice Chief Science Officer
SS Tranquility
User avatar
Ferre Flamand
Sciences - Lieutenant
Sciences - Lieutenant
Posts: 358
Joined: 211111.0543
Duty Post: Vice Chief Science Officer
Ship/Station Posted: SS Tranquility
Grid: Second Life
Location: Belgium
Has thanked: 185 times
Been thanked: 54 times
Contact:

220731.0140

Tranquility Station/Ops + Tranquility Science Lab - Stardate 22073102.30
Reporting Officer: Lt Ferre Flamand
Other Officers on Duty: 4 NPC's
Duty Log
Daily Scientific and Observation Report


Surface environmental conditions

Nitrogen = 77.08 percent
Oxygen = 20.16 percent
Argon = 0.87 percent
Neon, Helium, Krypton = 0.0008 percent
Carbon dioxide = 0.22 percent
Water vapor = 0 - 4 percent

Fauna and Flora = All specific data found in local database.
Daystar condition = Thermal radiation within acceptable margins. One active sunspot-grouping detected with low active flares. No communication interference can be expected. Warming-up sequence at normal rate within range.

Betelgeuse (Alpha Orionis) its variable magnitude intervals within range. Brightned by 0.02 magnitude in brightness.


Today's project : HD 28109 hosts a trio of transiting Neptunian planets including a near-resonant pair.

We report on the discovery and characterization of three planets orbiting the F8 star HD 28109, which sits comfortably in TESS’s continuous viewing zone. The two outer planets have periods of 56.0067±0.0003 d and 84.2597+0.0010−0.0008 d⁠, which implies a period ratio very close to that of the first-order 3:2 mean motion resonance, exciting transit timing variations (TTVs) of up to 60min⁠. These two planets were first identified by TESS⁠, and we identified a third planet in the TESSphotometry with a period of 22.8911±0.0004 d⁠. We confirm the planetary nature of all three planetary candidates using ground-based photometry from Hazelwood, ASTEP⁠, and LCO, including a full detection of the ∼9h transit of HD 28109 c from Antarctica. The radii of the three planets are Rb=2.199+0.098−0.10 R⊕⁠, Rc=4.23±0.11 R⊕⁠, and Rd=3.25±0.11 R⊕⁠; we characterize their masses using TTVs and precise radial velocities from ESPRESSO and HARPS, and find them to be Mb=18.5+9.1−7.6 M⊕⁠, Mc=7.9+4.2−3.0 M⊕⁠, and Md=5.7+2.7−2.1 M⊕⁠, making planet b a dense, massive planet while c and d are both underdense. We also demonstrate that the two outer planets are ripe for atmospheric characterization using transmission spectroscopy, especially given their position in the CVZ of UFS Space Telescope. The data obtained to date are consistent with resonant (librating) and non-resonant (circulating) solutions; additional observations will show whether the pair is actually locked in resonance or just near-resonant.


-- end log --

:communicator: Lt Ferre Flamand
Vice Chief Science Officer
SS Tranquility
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