It’s possible to have secret lives of Neutron Stars

GW170817 and Gaia Data Release 2: Systematic errors and accuracy of the VLBI Astrometry and X-ray afterglows

Lamb, G. P., Mandel, I. & Resmi, L. Late-time evolution of afterglows from off-axis neutron star mergers. Mon. Not. R. Astron. Soc. 481, 2581–2589 (2018).

Drout, M. R. et al. The implications for r-process nucleosynthesis were discussed by the light curves of the neutron star merger. Science 358, 1570–1574 (2017).

Andreoni, I. et al. Follow up of GW170817 and its electromagnetic counterpart by Australian-led observing programmes. Publ. Astron. Soc. Aust. 34, e069 (2017).

Lewin, W. and van der Klis are the authors of the Compact X-ray Sources. The Cambridge astrophysics series is No. 39. Press, 2006).

Bellini, A., Anderson, J. & Bedin, L. R. Astrometry and photometry with HST WFC3. II. Improved geometric-distortion corrections for 10 filters of the UVIS channel. Publ. Astron. Soc. ThePac 123, 622 was published in 2011.

Greisen, E. W. in Information Handling in Astronomy—Historical Vistas Astrophysics and Space Science Library Vol. 285 (ed. Heck, A.) 109–125 (Springer, 2003).

The comparison with Gaia Data Release 2 was made for systematics and accuracy of VLBI Astrometry. Astron. Astrophys. 634, A28 (2020).

Kovalev, Y. Y., Petrov, L. & Plavin, A. V. VLBI-Gaia offsets favor parsec-scale jet direction in active galactic nuclei. There is an Astron. Astrophys. 609, L1

Petrov, L., Kovalev, Y. Y. & Plavin, A. V. A quantitative analysis of systematic differences in the positions and proper motions of Gaia DR2 with respect to VLBI. The day was Mon. Not. R. Astron. There are a number of articles published in a single edition of 482 and 3023–3031.

Charlot, P. et al. The third realization is by very long baseline interferometry. Astron. In 2020 astrophys. 644 and A 159.

E., Lazzati, D. and M.J. were related. Afterglow light curves, viewing angle and the jet structure of γ-ray bursts. Mon. Not. There was R. Astron. 332 and 955 were published in 2002.

A new tool for detecting the dark energy and the gamma-ray bursts “Pac 116, 425 – 440”

Speagle, J. S. DYNESTY: a dynamic nested sampling package for estimating Bayesian posteriors and evidences. Mon. Not. R. Astron. Soc. 493, 3132–3158 (2020).

Soares-Santos, M. The Dark Energy Survey and The Dark Energy Camera GW-EM Collaboration et al. The opposite of the LIGO/Virgo merger. I. Discovery of the optical counterpart using the dark energy camera. Astrophys. J. 832, L16

Mangan, J., Dunwoody, R. & Meegan, C.; Fermi GBM Team. GRB 211211A: There was an observation of the Fermi GBM. GRB Coordinates Network, Circular Service, No. 31210 (2021).

Nicholl, M. There are tight multimessenger constraints for the neutron star equation of state and a forward model for lightcurve synthesis. Mon. Not. R. Astron. The report was published in 3016–3032

Can magnetar spin down power extend emission in some short GRBs? There was no activity on Mon. Not. R. Astron. 431 was published in the year 2013).

The effect of heating on accretion in compact object mergers. Mon. Not. R. Astron. Soc. 402, 2771–2777 (2010).

Adriani, O. Extended measurement of the cosmic-ray electron and positron spectrum from 11 GeV to 4.8 TeV with the calorimetric electron telescope on the International Space Station. Phys. Rev. Lett. 120, 261102 (2018).

GRB ike FuN: redshift estimation and Spi-acs/integrRAL detection. GRB Coordinates Network, Circular Service, No. 31230 (2021).

T. Matheson, et al. The first two months were for photometry and spectroscopy of GRB 030329. Astrophys. J. 599 was published in 2003

Hook, I. M. et al. The performance of the multi-object spectrograph in various modes. Publ. Astron. The name of the company is Soc. The article is entitled “Pac 116, 425–440”.

Labrie, K., Anderson, K., Cárdenes, R., Simpson, C. & Turner, J. E. H. DRAGONS – Data Reduction for Astronomy from Gemini Observatory North and South. There is a conference called the sasp conf. Ser. 523, 321 were published in 2019.

Lang, D., Hogg, D. W., Mierle, K., Blanton, M. & Roweis, S. Astrometry.net: blind astrometric calibration of arbitrary astronomical images. The Astron. J. 139, 1782–1800 (2010).

The Sloan Digital Sky Survey has a tool for reddening and recalibrating SFD. There are astrophys. J. 509, 103 (2011).

C.N. A., Willmer and others. The Deep Evolutionary Exploratory Probe 2 galaxy redshift survey: the galaxy luminosity function to z ~ 1. There are astrophys. J. 797, 832, and 825 were published in 2006

S L. Finkelstein is an author. The evolution of the galaxy rest-frame ultraviolet luminosity function over the first two billion years. Astrophys. J. 810, 71 (2015).

Nugent, A. E. et al. The distant, galaxy cluster environment of the short GRB 161104A at z ~ 0.8 and a comparison to the short GRB host population. There are astrophys. J. 904, 52 (2020).

Wright, E. L. et al. The WISE consists of a mission description and an on-orbit performance. Astron. J. 140, 1868- 81 was published in 2010.

Calura, F. et al. The dust-to-stellar mass ratio is a useful tool for studying the evolution of local and distant star-forming galaxies. Mon. Not. R. Astron. Soc. 465, 54–67 (2017).

Duffell, P. C., Quataert, E., Kasen, D. & Klion, H. Jet dynamics in compact object mergers: GW170817 likely had a successful jet. Astrophys. J. 866 was written on 3/12/2018.

M. W., T., Margalit, B., and B. D are all associated with multimessenger inference. Mon. Not. R. Astron. There were reports on the Soc. 482, 91 and 96.

Kasen, D., Metzger, B., Barnes, J., Quataert, E. & Ramirez-Ruiz, E. Origin of the heavy elements in binary neutron-star mergers from a gravitational-wave event. Nature 556, 80–84.

Khan, S. et al. The waves come from the black-hole. The second part of the story. A phenomenological model for the advanced detector era. The Phys. Rev. D 93 had a message in January 2016

Dietrich, T., Bernuzzi, S. & Tichy, W. Closed-form tidal approximants for binary neutron star gravitational waveforms constructed from high-resolution numerical relativity simulations. The first part of the article is devoted to Phys. Rev. D 96.

The book is titled O’Connor, B. et al. A tale of two mergers: constraints on kilonova detection in two short GRBs at z ~ 0.5. It will be Monday. Not. R. Astron. The following year, sso 500, 1279–128.

Moskvitin, A., Spiridonova, O., Belkin, S., Pozanenko, A. & Pankov, N.; GRB IKI FuN. GRB 211211A: SAO RAS optical observations. The GRB Coordinates Network is a circular service.

McMullin, J. P., Waters, B., Schiebel, D., Young, W. & Golap, K. CASA architecture and applications. In Astronomical Data Analysis Software and Systems XVI: Astronomical Society of the Pacific Conference Series Vol. 376 (eds Shaw, R. A. et al.) 127 (2007).

A python package is used to simplify Fermi-LAT analysis. In International Cosmic Ray Conference: International Cosmic Ray Conference Vol. 33, 2784 (2013).

Khangulyan, D., Aharonian, F. A. & Kelner, S. R. Simple analytical approximations for treatment of inverse Compton scattering of relativistic electrons in the blackbody radiation field. Astrophys. J. 783, 100 (2014).

Seeing a kilonova with the Cerro Tololo Inter-Area Inter-American Observatory: The case of a rare star pair

It is the first confirmed detection of a star system that can create a kilonova, when the stars in it collide and explode. The rare stellar pair is believed to be one of only about 10 like it in the Milky Way galaxy.

The Neil Gehrels Swift Observatory detected a huge X-ray flash in the same area where a hot, bright be-type star was located.

Astronomers were curious if the two could potentially be linked, so data was captured using the Cerro Tololo Inter-American Observatory’s 1.5-meter telescope in northern Chile.

One of those interested in using this data to learn more about the star was Dr. Noel D. Richardson, now an assistant professor of physics and astronomy at Embry-Riddle Aeronautical University.

Clarissa Pavao, an undergraduate at the university, asked Richardson if he had any projects she could work on to gain experience with astronomy research. He shared the telescope data with her and throughout the pandemic, Pavao learned how to work with the data from the telescope in Chile and clean it up to reduce distortion.

Be stars tend to have disks of matter around them, but you can see the elements in the star through the telescope. “It’s hard to see directly through all that stuff.”

Source: https://www.cnn.com/2023/02/01/world/supernova-rare-star-pair-scn/index.html

A supernova rare star pair in the path of a massive, energy-rich, long-lived spherical star in CPD-29 2176

But that orbit wasn’t what they were expecting. In a circular shape, the stars whirl around one another. In CPD-29 2176, one star orbits the other in a circular pattern that repeats about every 60 days.

The two stars, a larger one and a smaller one, were whirling around one another in a very close orbit. Richardson said that the larger star was releasing material onto the smaller star, which grew from 8 to 19 times the mass of our sun. Our sun is 333,000 times larger than Earth.

The main star became smaller and smaller while building up the secondary star — and by the time it had exhausted all of its fuel, there wasn’t enough to create a massive, energetic supernova to release its remaining material into space.

Richardson said that the star had so little energy that it did not have enough to kick its elliptical form into motion.

The remnants of a dense star that was left after an ultra-stripped supernova are now in the path of a massive star. The stellar pair will not change their configuration for about 6 to 7 million years. It releases a disk of gas to balance itself and make sure it don’t rip itself apart because both mass and angular momentum were transferred to Be star.

Eventually, the secondary star will also burn through its fuel, expand and release material like the first one did. The star system will release the material through space because it can’t easily be piled up on the neutron star. The secondary star will most likely experience a lackluster supernova, and turn into a neutron star.

Source: https://www.cnn.com/2023/02/01/world/supernova-rare-star-pair-scn/index.html

The Birth and Death of the Universe. Stellar Genealogy: Searching for Evidence of Massive Star Mergers on a Cosmological Scale

“Those heavy elements allow us to live the way that we do. For example, most gold was created by stars similar to the supernova relic or neutron star in the binary system that we studied. Richardson believes that astronomy makes our understanding of the world and our place in it better.

“When we look at these objects, we’re looking backward through time,” Pavao said. We get to know a lot more about the universe’s origin, which will help us chart out where our solar system is headed. As humans, we started out with the same elements as these stars.”

Richardson and pavao worked with a physicist at the University of Auckland who is an expert on star systems and their evolution. The study estimated there are about 10 star models in the whole of the galaxy, similar to the one reviewed by Eldridge.

Next, the researchers want to work on learning more about the Be star itself, and hope to conduct follow-up observations using the Hubble Space Telescope. Pavao is hoping to complete her degree and continue to work on space physics research using the new skills she has acquired.

The past can be studied on a different scale than archaeologists or paleontologists. When astronomers catch a glimpse of an unusual signal in the sky, perhaps the light from a star exploding, Stevance takes that signal and rewinds the clock on it by billions of years. Working at the University of Auckland in New Zealand, she traces the past lives of dead and dying stars, a process she calls stellar genealogy. She said there is a lot of drama in the lives of stars.

Researchers don’t know how common these mergers are, and they can’t tell whether they are responsible for creating all the heavy elements in the universe, or just a fraction. astrophysicists could answer questions like how old the universe is if they observed more of these mergers. This is where stellar genealogy can help.

The work describes the interaction between the two stars after they burned out their fuel. They started tens of millions of kilometers apart but are not very far apart from each other. Each star’s exterior was surrounded by gas known as a stellar envelope. The models determined that over the stars’ lifetimes one star’s envelope engulfed the other and their outer gases merged to become a single shared envelope.

Barnes, J. There is an effect on the light curves of radioactively powered Transients from compact object mergers. Astrophys. J. 775, 18.

C.Nicolaou and several others were involved in a project. The estimation of the Hubble constant from standard sirens is affected by peculiar velocities. The day will be on Mon. Not. R. Astron. The year 2020 is Soc. 499, 90–97

Collins, S. et al. There are variations in Type Ia supernovae due to different core. Synthetic observables are the things and He shell mass. The day was Mon. Not. R. Astron. Soc. 517, 5289–5302 (2022).

Dessart and Hillier used type II supernovae and expanding photoosphere to determine distance. Astron. Astrophys. 439, 671–685 (2005).

Just, O. and et al. Neutrino absorption in black hole accretion discs: a rare event

Just, O. and et al. The black hole accretion discs have Neutrino absorption in them. Mon. Not. R. Astron. Soc. 509, 1377–1412 (2021).