Asteroseismology of fast-rotating stars : the contribution of two-dimensional calculations
Giovanni Mirouh (University of Surrey, United Kingdom)
Massive stars directly and indirectly drive the chemical enrichment of the interstellar medium. These stars usually exhibit rapid differential rotation, and are known pulsators. Because of rotation, oscillations in these stars are hard to interpret and modes cannot be readily identified, preventing us from using well-established asteroseismology techniques. In this talk, I will present recent advances in the description of oscillations in such stars. After a general introduction, I will describe low-frequency oscillations in presence of differential rotation: this rotation affects their propagation and is even responsible for the excitation of some modes. I will then discuss higher-frequency oscillations, that can be split into different categories. Using a convolutional neural network, it was possible to classify these modes automatically and derive a scaling law linking regular patterns in the spectra to stellar properties. Finally, I will suggest future work needed for realistic seismic modelling of fast-rotating stars.
A Novel Modeling of Magneto-Rotating Stellar Evolution
髙橋 亘 / Koh Takahashi (Albert-Einstein-Institut, Potsdam, Germany)
About 10% of massive and intermediate-mass main-sequence stars posses strong surface magnetic fields, and the magnetic massive stars may be progenitors of strongly magnetized neutron stars known as magnetors. However, the evolution of magnetic fields in stellar interiors remains a big open question for the stellar evolution theory. We are developing a new stellar evolution code which is capable to follow a long-timescale evolution of stellar magnetism. Because of the far different timescales between the MHD and the evolutionary times, high degree of simplification in the modeling is inevitable. First, we assume that the configuration of the stellar magnetic field can be approximated by axially symmetric toroidal + poloidal components, which explicitly has only a radial dependence. Then the evolution of the two component magnetic field is described by the mean-field dynamo equation. The new formalism self-consistently includes the effects of omega-dynamo, which results from large scale shear in the rotation flow, magnetic dissipation, and angular momentum transfer due to magnetic stress. We will present our preliminary results and discuss how the model can be verified by observations.
The Formation of Rings and Gaps in Magnetized Wind-Launching Disks
Scott Suriano (University of Tokyo)
Radial substructures in circumstellar disks are now routinely detected by state-of-the-art observational facilities. There is also growing evidence that large-scale magnetic fields threading disks are responsible for launching disk winds and driving accretion. We investigate how rings and gaps form in magnetized disks through non-ideal MHD simulations. In axisymmetric 2D simulations including either Ohmic resistivity or ambipolar diffusion (AD), prominent features form in the disk surface density with a strong radial variation of the poloidal magnetic flux relative to the mass. Regions with low mass-to-flux ratios accrete quickly and lead to the development of gaps, whereas regions with higher mass-to-flux ratios accrete more slowly, allowing matter to accumulate and form dense rings. Specifically, in the AD-dominated disks, the radial variation of the magnetic flux is set by the reconnection of a highly elongated poloidal magnetic field across a thin midplane current sheet, through which fast laminar accretion occurs. We extend the simulations of AD-dominated disks to 3D and find that rings and gaps still develop naturally from the same basic mechanism that was identified in 2D. The rings and gaps remain stable in 3D for a few thousand orbital periods at the inner edge of the simulated disks, making them attractive sites for trapping large grains that would otherwise be lost to rapid inward radial migration.
WR DustERS: a JWST-ERS program to resolve the nature of dust in Wolf-Rayet binary winds
Ryan M. Lau (ISAS/JAXA)
Thermal infrared (IR) emission from dust is a key probe of the evolution and death of short-lived, massive stars. Dust itself is a key component of the interstellar medium; however, the dominant channels of dust production throughout cosmic time are uncertain. In this talk, I will discuss our JWST Director’s Discretionary Early Release Science (DD ERS) program, where we will investigate the formation mechanism and chemical composition of dust formed in the colliding winds of a Carbon-rich Wolf-Rayet (WC) binary. With dust production rates ranging from 10-8 – 10-6 M☉/yr, such massive stellar binaries may have a significant influence on the dust abundance of galaxies in both the local and early Universe. Dust abundances, composition and formation pathways in the hostile and luminous environment around WC+OB binaries are, however, uncertain due to observational challenges in achieving both high spatial resolution and sensitivity in the mid-IR. Our planned JWST/MIRI+MRS and NIRISS+AMI observations of the archetypal periodic dust forming Wolf-Rayet binary system WR140 will address these uncertainties and also demonstrate the utility of these observing modes for IR bright targets with faint extended emission.
Inefficient Magnetic Accretion Heating in Protoplanetary Disks
森 昇志 (天文学教室) / Shoji Mori (Department of Astronomy)
The structures of the inner region of protoplanetary disks are essential for understanding the formation process of terrestrial planets. The gas temperature in the region is thought to be determined by accretion heating, which is conventionally attributed to turbulent dissipation. However, recent studies have suggested that the inner disk (a few AU) is largely laminar, with accretion primarily driven by magnetized disk winds, as a result of nonideal magnetohydrodynamic (MHD) effects from weakly ionized gas, suggesting an alternative heating mechanism by Joule dissipation.
We perform local stratified MHD simulations including nonideal MHD effects and investigate the role of Joule heating and the resulting disk vertical temperature profiles. We find that most of the accretion energy is used to drive disk winds, with the remaining for Joule heating that typically occurs at several scale heights above the midplane, making the midplane temperature much lower than that with the conventional viscous heating model. Our results suggest that the midplane temperature in the inner PPDs is almost entirely determined by irradiation heating. We also discuss the evolution of the water snow line based on our results and the formation process of the Earth.
The strongest magnetic fields in sunspots
岡本 丈典 (国立天文台) / Joten Okamoto (National Astronomical Observatory of Japan)
Sunspots are concentrations of magnetic fields on the solar surface. Then, where is the strongest field in each sunspot ? It is generally located in an umbra, but sometimes stronger fields are found outside umbrae, such as a penumbra and a light bridge. The formation mechanism of such strong fields outside umbrae is still puzzling. Now we have numerous high-quality datasets taken with the Hinode/Spectro-Polarimeter over 10 years, which motivate us to address this question via a statistical analysis of strongest fields in sunspots. Hence, we complied a ranking list of active regions by their largest field strengths and investigated conditions for appearance or formation of strong magnetic fields. In this seminar, we will introduce a sunspot with a field strength of 6250 G as a case study, and then discuss the key features to produce strong fields in a statistical sample.
First M87 Event Horizon Telescope Results: The Shadow of the Supermassive Black Hole
水野 陽介 / Yosuke Mizuno (Goethe University Frankfurt)
The Event Horizon Telescope (EHT) has mapped the central compact radio source of the elliptical galaxy M87 at 1.3 mm with unprecedented angular resolution. These images show a prominent ring with a diameter of ~40 micro-arcsecond, consistent with the size and shape of the lensed photon orbit encircling the “shadow” of a supermassive black hole. The ring is persistent across four observing nights and shows enhanced brightness in the south. Here we consider the physical implications of the asymmetric ring seen in the 2017 EHT data. To this end, we construct a large library of models based on general relativistic magnetohydrodynamic simulations and synthetic images produced by general relativistic ray tracing. We compare the observed visibilities with this library and confirm that the asymmetric ring is consistent with earlier predictions of strong gravitational lensing of synchrotron emission from a hot plasma orbiting near the black hole event horizon. Overall, the observed image is consistent with expectations for the shadow of a spinning Kerr black hole as predicted by general relativity. If the black hole spin and M87’s large scale jet are aligned, then the black hole spin vector is pointed away from Earth. Models in our library of non-spinning black holes are inconsistent with the observations as they do not produce sufficiently powerful jets. We also briefly discuss the possibility of the alternatives to a black hole for the central compact object.
Type Ia supernova progenitors
山口 弘悦 (宇宙科学研究所) / Hiroya Yamaguchi (ISAS/JAXA)
Type Ia supernovae, widely believed to result from thermonuclear explosions of white dwarfs, are extremely important phenomena in the Universe, owing to their roles as distance indicators in cosmology and major sources of iron. However, many of their fundamental aspects, e.g., how their progenitors evolve and explode, remain elusive. I will review recent observational and theoretical work addressing this issue, and discuss future prospects for both electromagnetic and gravitational wave observations.
How AGN radiative feedback may shape black hole-galaxy co-evolution
石橋 和貴子 / Wakiko Ishibashi (University of Zurich)
Active Galactic Nucleus (AGN) feedback is widely invoked in galaxy evolutionary models, while evidence of such AGN feedback in action is now observed in the form of galactic outflows. However, the physical mechanism driving AGN feedback remains ill-understood, and whether galactic outflows are powered by jets, winds, or radiation, is still a source of much debate. We consider AGN feedback driven by radiation pressure on dust. We show that such radiative feedback is capable of accounting for the observed dynamics and energetics of galactic outflows, provided that radiation trapping is properly taken into account.
Feedback from the central black hole is usually invoked to quench star formation in galaxies (the standard negative feedback paradigm). We consider the alternative possibility of triggering star formation in the host galaxy, within the feedback-driven outflows (a form of positive feedback). Such “AGN feedback-driven star formation” may contribute to the size and morphological evolution of galaxies over cosmic time. Recently, there has been growing observational evidence for such star formation occurring inside galactic outflows. I will discuss the multiple roles of AGN feedback in galaxy evolution, and how radiative feedback may ultimately shape the co-evolutionary path.
How to Create Flare-productive Sunspots?
鳥海 森 (宇宙科学研究所) / Shin Toriumi (ISAS/JAXA)
Solar flares, especially the strong ones, emanate from active regions including sunspots, where high magnetic non-potentiality resides in a wide variety of forms. In this talk, I will introduce some of our recent works on the flare-productive sunspots: (1) the statistical survey on flare-productive spots [Toriumi et al. 2017]; (2) the 3D MHD simulations of such flaring spots [Toriumi & Takasao 2017]; and (3) the flare loop modeling and reproduction of SXR light curves [Reep & Toriumi 2017]. Based on these studies, we show that the twist and interaction of subsurface magnetic fields give rise to the flare-producing sunpots. In this talk, I will also discuss possibilities to apply our solar knowledge to the investigation of stellar activities.
GALACTIC WINDS: Physics, Phenomenology, and Implications
Timothy Heckman (Johns Hopkins University)
I will review galactic winds driven by populations of massive stars. I will describe the basic physics that drives winds and dictates their impact on the interstellar and circum-galactic medium. I will describe observations of the multi-phase outflow in the proto-typical starburst galaxy M 82. I will then discuss the systematic dependence of wind properties on such key parameters as the star-formation-rate, galaxy size, and mass (circular velocity), and show that there explain the strong rise in the incidence rate of winds with redshift. I will also compare these empirical scaling relations with sub-grid recipes commonly adopted in models and simulations. Finally, I will describe observations that demonstrate the impact of winds on the chemical evolution of galaxies and on the properties of the circum-galactic medium.
Machine Learning for Classification of Astronomical Data
Tilman Hartwig (物理学専攻 / Department of Physics)
I will give an overview of machine learning techniques and present decision trees as very efficient machine learning tool to classify astronomical data. A labelled training sample is split according to available features by requiring that each split minimises the information entropy of the assigned classes. This elegant mathematical formulation allows us to construct decision trees with supervised learning, which can then be applied to classify new observations.
Eventually, I will present recent results of my own research: by classifying the chemical abundance patterns of metal-poor stars in the Milky Way, we can derive the multiplicity of the first generation of stars in the Universe. Furthermore, this approach provides the feature importance to identify crucial chemical elements to classify metal-poor stars, which can be used to optimise future spectroscopic surveys of Milky Way stars.
Direct Detection of Nano-Herz Gravitational Waves with Pulsar Timing Array
高橋 慶太郎 (熊本大学) / Keitaro Takahashi (Kumamoto University)
Pulsar timing array is a unique way to detect gravitational waves of nano-Hz frequencies and will greatly contribute to the multi-wavelength gravitational-wave astronomy. The major sources of nano-Hz are super-massive black hole binaries and cosmic strings, and we can probe structure formation of the universe in a different way from the other methods. In this talk, I will review the basic idea of pulsar timing array and the current status, and then give prospects for a future project, SKA (Square Kilometre Array).
The shadow of M87’s super-massive black hole revealed by EHT
本間 希樹 (国立天文台) / Mareki Honma (NAOJ)
On 10 April 2019, the first-ever image of a black hole shadow has been released. The image, taken by the Event Horizon Telescope toward M87’s core, shows a ring-like structure corresponding the photon-sphere of the black hole. The image also shows a clear depression of its intensity at the ring center, the shadow of a black hole, visually demonstrating for the first time that even light cannot escape from a black hole. In this talk, I would like to summarize the EHT results on M87, by describing the properties of images as well as details of observations and data analysis.
Young star clusters: a nursery of merging binary black holes
Ugo Niccolò Di Carlo (University of Insubria, Italy)
Searching for distinctive signatures, which characterize different formation channels and environments of binary black holes (BBHs), is a crucial step towards the interpretation of current and future gravitational wave detections. In this talk, I will discuss the formation of merging BBHs in young star clusters (SCs), which are the nursery of massive stars. In particular, I will show the results of a large set of N-body simulations of SCs with a large primordial binary fraction and novel population-synthesis prescriptions. The simulated SCs have fractal initial conditions, to mimic the clumpiness of star forming regions. I will discuss the impact of star cluster dynamics on the properties (total masses, mass ratios and delay times) of merging BBHs. More than 50% of merging BBHs formed by dynamical exchange in our simulations. BBHs formed via exchanges are significantly more massive than BBHs formed from primordial binaries, reaching chirp masses larger than 30 Msun. In our simulations, dynamical exchanges are the only channel able to form merging BBHs similar to GW170729, the most massive gravitational wave event observed by LIGO-Virgo. Finally, stellar collisions lead to the formation of intermediate mass black holes (IMBHs) with mass up to 440 Msun. IMBHs represent <~ 0.1 % of all black holes in our simulations.
Constraining Progenitor Models and Cosmology with New Localizations of Fast Radio Bursts
J. Xavier Prochaska (University of California, Santa Cruz)
I will report on a set of new, well-localized (<1”) fast radio bursts (FRBs) discovered by the ASKAP telescope. Nearly each of these events is coincident with a luminous galaxy which we designate as the host. The properties of these host galaxies and the spatial distribution of the FRBs within them rule out several classes of models proposed for FRBs. Spectra of the galaxies establish the FRB redshifts, offering a first assessment of the dispersion measure vs. redshift relation. This yields a new estimate of the cosmic baryon density for the low-z universe, consistent with measurements from BBN and the CMB, i.e. the so-called “missing” baryons have been found! Last, we analyze the rotation measure and pulse width of one FRB to study the magnetic field and density of gas in a foreground galaxy halo.
The multiple eruptions of Eta Carinae and its evolution
平井 遼介/Ryosuke Hirai (University of Oxford)
Eta Carinae is one of the most extraordinary stars known in our galaxy, having many peculiar properties. One of the most prominent features is that it is surrounded by bipolar lobes called the Homunculus nebula. This nebula originated from the Great Eruption in 1844 that was visible to the naked eye. It is also known that Eta Car had other small eruptions centuries before the Great Eruption, where smaller ejectiles were emitted with ~300 year intervals. Eta Car itself has extremely strong winds reaching mass-loss rates of Mdot~10-3M⊙/yr, which interacts with the wind from a companion star that orbits in a 5.5 yr period. Many attempts have been made to understand the formation of Eta Car and its many peculiar properties, but most models have failed to explain all features self-consistently.
Here we propose a new scenario starting with a hierarchical triple system. The system becomes unstable after mass-transfer in the inner binary and reaches large eccentricities. Each periastron interaction peels off material off the primary star and ejects them as outer ejecta. Then the instability eventually triggers a merger, leading to the Great Eruption and formation of a bipolar nebula. In this talk I will show results of 2.5D hydrodynamical simulations of a stellar merger and show that it can reproduce the observed Homunculus nebula well. I will also discuss how close periastron encounters in triple systems can reproduce the Outer ejecta via n-body simulations.
Understanding the formation of Eta Carinae helps us understand the formation and evolution of LBVs in general, and possibly many other peculiar objects.
Gas in debris disks: a new tool to study exoplanetary systems
Gianni Cataldi (Department of Astronomy)
Debris disks have traditionally been considered gas-poor remnants of dispersed protoplanetary disks. However, ALMA has recently detected CO in a number of debris disks, in some cases with CO masses comparable to protoplanetary levels. The origin of this gas is still under debate: both a primordial (leftover from the protoplanetary phase) and secondary (evaporation of exocomets) origin have been proposed. In this talk, I will present ALMA follow-up observations of neutral carbon, a photo-dissociation product of CO. Carbon allows us to constrain the evolution and dynamics of these systems in new and interesting ways. For example, we used C observations to reject previous claims that the clumpy structure observed in the beta Pictoris debris disks is due to an additional planet interacting with the disk. I will also show that carbon observations are crucial to constrain the secondary origin scenario.
FRB cosmology and [CII] detection of a GRB host galaxy
橋本 哲也 (台湾国立清華大学）/ Tetsuya Hashimoto (National Tsing Hua University, Taiwan)
I will present my recent papers on (i) the luminosity-duration relation of fast radio bursts (FRBs) and (ii) ALMA observations of Gamma-Ray Burst (GRB) host galaxies. Brief summaries of each paper are as follows.
(i) Luminosity-duration relation of fast radio bursts
We discovered an empirical correlation between luminosity and duration of FRBs. We propose a new distance measure using the relation of FRBs, which can reach more distant Universe than type Ia supernovae in quantity. This method can potentially reveal the time variability of the dark energy, which is one of the central foci of observational cosmology.
(ii) SFRs of two GRB host galaxies at z~2 and a [CII] deficit observed with ALMA
We discovered a new parameter to characterize GRB host galaxies, [CII] deficit, by overcoming a serious dust-extinction problem of GRB host galaxies. Possible parameters controlling the deficit include the metallicity, initial mass function, and gas density.
A new approach to generate realistic star clusters from hydrosimulations
Alessandro Ballone (Astronomical Observatory of Padova)
Initial conditions are one of the most critical issues in the numerical modelling of star clusters. Most direct N-body simulations of star clusters adopt idealized initial conditions: spherically symmetric, gas-less and virialised. Hydrodynamical simulations of molecular cloud collapse suggest that clustered star formation is quite different from that. A natural approach would thus be to use hydrodynamical simulations of molecular cloud fragmentation to inform the initial conditions of star cluster simulations. However, this procedure is extremely difficult to implement: because of the high computational cost of hydro-simulations, their currently feasible mass/spatial resolution never allows to follow star formation on the smallest possible scales, hence, e.g., to sample a complete initial mass function. I will present a new approach to link the output of hydrodynamic simulations to the input of direct N-body ones. The new method is based on generating stars by splitting “hydrodynamical” sink particles in post-processing, so to ensure that any chosen mass function is recovered. This approach has the advantage of producing a more realistic population of star clusters, both in terms of their internal kinematics and initial spatial distribution, compared to what has been so-far often adopted for N-body studies in literature.
An Insight into the galactic hosts and environments of merging compact binary objects
Soheb Mandhai (University of Leicester)
The coalescence of two compact objects, such as a neutron star paired with either a black-hole or secondary neutron star, are potential sources for the emission of observable gamma-ray bursts, and gravitational waves. By tracing a population of stellar binaries within hydrodynamically simulated galaxies, we can observe the properties of host galaxies and the environment of the binary upon merging. Furthermore, we consider a distribution of binaries with natal kick velocities that may be enough to eject them from the potentials of their host galaxies. From an observational perspective, localising the host galaxies for these ejected binaries can be difficult. Using a population of well-localised short-duration gamma-ray bursts (SGRBs) we give constraints on the association with galaxies within 200 Mpc assuming a maximum on-sky projection of 200 kpc. This gives an upper limit on the all-sky rate of SGRBs of 4 per year for d< 200 Mpc.
The Origins Space Telescope
左近 樹（天文学教室）/Itsuki Sakon (Department of Astronomy)
The Origins Space Telescope (Origins) is one of the four mission concepts studied for the 2020 US astrophysics decadal survey in the framework of Science and Technology Definition Team (STDT) activity. The Origins will trace the history of our origins: it investigates (1) how galaxies form stars, make metals, and grow their central supermassive black holes from reionization to today, (2) how the conditions for habitability develop during the process of planet formation, and (3) whether the planets orbiting M-dwarf stars support life.
In the baseline design described in the final study report, the Origins operates from ~2.8 to 590µm and is more than 1000 times more sensitive than prior far-infrared missions due to its cold (~4.5K) aperture with a collecting area of ∼25m2 (equivalent to that of JWST). The Origins has three baseline instruments: (1) Origins Survey Spectrometer (OSS) covering wavelength from 25 to 588µm with the spectral resolution power R=300-43,000 and from 100 to 200µm with R=325,000, (2) Far-infrared Imager and Polarimeter (FIP) with imaging and polarimetric capability with 50 or 250µm bands, (3) Mid-Infrared Spectrometer Camera Transit (MISC) designed to achieve ultra-stable transit spectroscopy covering 2.8-20µm with R=50-295.
JAXA has led the study of the MISC together with NASA/Ames.The highest ever spectro-photometric stability of MISC is achieved by employing densified pupil spectrometer design (Matsuo et al. 2016), which provides the Origins with the capabilities to characterize the atmospheres of exoplanets around nearby K- and M-dwarfs and to identify potentially habitable worlds.
The results of the 2020 decadal survey will be announced in the beginning of 2021.
Investigation of Interstellar PAH molecules as carriers for mid-infrared emission bands
Mridusmita Buragohain (Department of Astronomy)
Interstellar Polycyclic Aromatic Hydrocarbon (PAH) molecules exist in diverse forms depending on the local physical environment of the Interstellar Medium (ISM). Formation of ionized PAHs (anions and cations) is favorable in the extreme condition of the ISM. Besides its pure form, PAHs are likely to exist in substituted forms, for example, PAHs with functional groups, nitrogenated PAHs, protonated and deuteronated PAHs, etc. The spectral evidence of PAH molecules and its variants in the ISM are observed via the mid-infrared emission bands, particularly at 3.3, 6.2, 7.7, 8.6, 11.2 and 12.7 μm. These bands, also known as ‘Aromatic Infrared Bands (AIBs)’ are widely present in the ISM and arise from the vibrational relaxation of PAH molecules on absorption of background UV photons. However, the exact form of PAH molecules that are responsible for the AIBs is still ambiguous. Here, we discuss a few of the possible forms of interstellar PAH molecules (for example: deuteronated and nitrogenated PAHs) as carriers for AIBs. Density Functional Theory (DFT) calculation on several classes of PAHs is employed to study its spectral characteristics in infrared. We compare our results with observations in quest of any correlation that establishes its presence in the ISM.
Revealing the Origin of Violent Stellar Transients from Fast Radio Bursts and Magnetars
山崎 翔太郎（天文学教室）/Shotaro Yamasaki (Department of Astronomy)
Transient astrophysical phenomena reveal the violent and capricious nature of the Universe, enabling us to probe extreme realms of physics that were not anticipated prior to their discovery. Fast radio bursts (FRBs) are one of such enigmatic transients with millisecond-duration bright radio flashes originating from beyond our galaxy. Most of FRBs have not been observed to repeat and such non-repeating FRBs may be explained by the pulsar-like emission expected at the time of the binary neutron star (BNS) merger. By using numerical-relativity simulations of a BNS merger, we examined this scenario with emphasis on the spacial distribution of the matter ejected during the coalescence, which may prohibit the FRB signal to propagate. We show that the formation of ejecta occurs about 1 ms after the rotation speed of the merged neutron star becomes high enough to produce an FRB. Furthermore, we propose a new scenario that a super young (1-10 yrs-old), fast-rotating massive neutron star left after the BNS merger could be the origin of repeating FRBs like FRB 121102. Magnetars, a class of highly magnetized neutron stars, are known to exhibit flaring activities in X-rays and gamma-rays with luminosities over ten orders of magnitude, which may be related to FRBs. Large amounts of magnetic energy are released as an electron and positron pair plasma, observable as magnetar flares. While most of theoretical progresses have been made in the early times, our understanding remains incomplete. In the second half of this talk, I will present our recent progress on the emission mechanisms for magnetar flares that includes (1) the relationship between short bursts (frequent but less energetic flares) and radio pulsations, and (2) the spectral modeling of intermediate and giant flares (rare but powerful flares).
Formation of massive galaxies in the early Universe and their multi-wavelength radiative properties
矢島 秀伸（筑波大学）/Hidenobu Yajima (University of Tsukuba)
Recent observations have successfully detected UV or infrared fluxes from galaxies at the epoch of reionization. However, the relation between the radiative properties and galaxy evolution has not been understood yet. Combining cosmological hydrodynamics simulations and radiative transfer calculations, we study the formation mechanism of galaxies and the origin of their radiative properties. We find that most of gas and dust are evacuated from star-forming regions due to supernova feedback. We show that galactic outflow allows UV photons to escape from galaxies. As halo mass increases, star- forming regions are covered by dusty gas, resulting in the formation of infrared bright galaxies. In my talk, we also show galaxy evolution in protocluster regions where many massive galaxies can form even in the early Universe. We show that massive dusty galaxies form along large-scale filamentary structure in the protocluster regions and the cosmic filaments emit Lyman-alpha cooling radiation.
Using stellar dynamics to connect the star formation and multi-message observations
Long Wang（Department of Astronomy）
Few-body dynamics plays an important role in the evolution of star clusters. Stars can escape the birth place after strong encounters with binaries. Perturbed binaries can merge to become more massive stars. Such few-body interactions also influence the energy flux of the stellar systems and determine the morphology and survival timescale of the clusters. I will show two examples how few-body dynamics can affect the feedback of star formation. This is especially related to the multiple stellar populations observed in the young star clusters like Orion Nebula Cluster and old globular clusters. On the other hand, the stellar-mass black hole is not only the progenitors of gravitational waves (GWs), but can significantly affect the long-term evolution of star clusters. Thus, by using stellar dynamics, we may construct a bridge to connect the initial mass function, primordial binaries and triples of young and old star clusters to the present observations from ALMA, Gaia and GW detectors.
Chasing the most distant objects
井上 昭雄（早稲田大学）/Akio Inoue (Waseda University)
Searching for the most distant objects is important. Due to the limited time before the observed epoch, these objects can put the most stringent constraint on the structure formation in the Universe. Recently, we have reported some discoveries of such objects with the world cutting-edge astronomical facilities including the Atacama Large Millimetre/submillimetre Array (ALMA). In this talk, I will present a review of some of the most distant objects which include the most distant oxygen, the most distant emission line and the most distant passive galaxy candidates. I will also discuss a future space mission to find the first-generation galaxies at z>15.
Are long-term N-body simulations reliable?
David Hernandez (Harvard-Smithsonian Center for Astrophysics)
Astrophysicists rely on solution for the N-body problem for a myriad of dynamics problems, from those in dark matter dynamics to those in planetary dynamics. Over 50 years ago, Miller found that errors in our simulations of the N-body problem grow exponentially in time. So why should one trust any such simulation over long times? In this talk, I explore a two-planet planetary system. The allowed motion over long times can be estimated by recent results from Hadden & Lithwich (2018). I find conventional integration methods are as accurate as fancier symplectic methods. In fact, a higher order symplectic method gave wrong statistics.