The version 3.0.26 beta is online

Version 3.0.26 offers new features like the support of eyepieces whose field can be represented on maps.

Under Android, it is also possible to activate a video mode allowing to overlay the images generated by WinStars with those coming from the camera located at the back of the device.

The icon system has also been revised for the Android mobile version.

Oumuamua, the Strange Interstellar Asteroid

Oumuamua is the first known interstellar object to pass through the Solar System. Formally designated 1I/2017 U1, it was discovered by Robert Weryk using the Pan-STARRS telescope at Haleakala Observatory, Hawaii, on 19 October 2017, 40 days after it passed its closest point to the Sun. When first seen, it was about 33,000,000 km (21,000,000 mi; 0.22 AU) from Earth (about 85 times as far away as the Moon), and already heading away from the Sun. Initially assumed to be a comet, it was reclassified as an asteroid a week later, and finally (6 November 2017) as the first of the new class of interstellar object.

Oumuamua is a small object, estimated to be about 230 by 35 meters (800 ft × 100 ft) in size. It has a dark red color, similar to objects in the outer Solar System. ʻOumuamua showed no signs of a comet tail despite its close approach to the Sun, and has significant elongation and rotation rate, so it is thought to be a metal-rich rock with a relatively high density. ʻOumuamua is tumbling rather than smoothly rotating, and it is moving so fast relative to the Sun that there is no chance it originated in the Solar System. It also means that ʻOumuamua cannot be captured into a solar orbit, so it will eventually leave the Solar System and resume traveling in interstellar space. ʻOumuamua’s system of origin and the amount of time it has spent traveling amongst the stars are unknown.

Oumuamua in WinStars 3

As the first known object of its type, ʻOumuamua presented a unique case for the International Astronomical Union, which assigns designations for astronomical objects. Before its true nature was known it was classified as comet C/2017 U1 and later as asteroid A/2017 U1. Once it was unambiguously identified as coming from outside the Solar System a new designation was created: I for Interstellar object. ʻOumuamua, as the first object so identified, was designated 1I, with rules on the eligibility of objects for I-numbers and the names to be assigned to these interstellar objects yet to be codified. The object may be referred to as 1I; 1I/2017 U1; 1I/ʻOumuamua; or 1I/2017 U1 (ʻOumuamua).

The name comes from Hawaiianʻoumuamua, meaning ‘scout’, (from ʻou, meaning ‘reach out for’, and mua, reduplicated for emphasis, meaning ‘first, in advance of) and reflects the way this object is like a scout or messenger sent from the distant past to reach out to us. The first character is a Hawaiian ʻokina, not an apostrophe, and is represented by a single quotation mark and pronounced as a glottal stop; the name was chosen by the Pan-STARRS team in consultation with Kaʻiu Kimura and Larry Kimura of the University of Hawaii at Hilo.

Before the official name was decided upon, the name Rama was suggested, the name given to an alien spacecraft discovered under similar circumstances in the science fiction novel Rendezvous with Rama (1973) by Arthur C. Clarke.

ʻOumuamua is the first known interstellar object to visit the Solar System and it appears to come from roughly the direction of the star Vega in the constellation Lyra. The incoming direction of motion of ʻOumuamua is 6° from the solar apex (the direction of the Sun’s movement relative to local stars), which is the most likely direction for approaches from objects outside the Solar System. On 26 October, two precovery observations from the Catalina Sky Survey were found dated 14 and 17 October. A two-week observation arc had verified a strongly hyperbolic trajectory. It has a hyperbolic excess velocity (velocity at infinity) of 26.33 km/s (58,900 mph), its speed relative to the Sun when in interstellar space.

By mid November, astronomers were certain that it was an interstellar object. Based on observations spanning 34 days, ʻOumuamua’s orbital eccentricity is 1.20, the highest ever observed. An eccentricity above 1.0 means an object exceeds the Sun’s escape velocity, is not bound to the Solar System, and may escape to interstellar space. While an eccentricity slightly above 1.0 can be obtained by encounters with planets, as happened with the previous record holder C/1980 E1, ʻOumuamua’s eccentricity is so high it could not have been obtained through an encounter with any of the Sun’s planets, known or unknown. Even undiscovered planets, if any exist, could not account for ʻOumuamua’s trajectory – any undiscovered planet must be far from the Sun and hence moving slowly according to Kepler’s laws of planetary motion. Encounters with such a planet could not boost ʻOumuamua’s speed to the observed value, and therefore ʻOumuamua can only be of interstellar origin. ʻOumuamua entered the Solar System from above the plane of the ecliptic. The pull of the Sun’s gravity caused it to speed up until it reached its maximum speed of 87.71 km/s (196,200 mph) as it passed below the ecliptic on 6 September and made a sharp turn upward at its closest approach to the Sun (perihelion) on 9 September at a distance of 0.255 AU (38,100,000 km; 23,700,000 mi) from the Sun, i.e., about 17% closer than Mercury’s closest approach to the Sun. The object is now heading away from the Sun (towards Pegasus) at an angle of 66° from the direction of its approach.

On the outward leg of its journey through the Solar System, ʻOumuamua passed below the orbit of Earth on 14 October at a distance of approximately 0.1616 AU (24,180,000 km; 15,020,000 mi) from Earth, and went back above the ecliptic on 16 October and passed above the orbit of Mars on 1 November. It will pass above Jupiter’s orbit in May 2018, Saturn’s orbit in January 2019, and Neptune’s orbit in 2022. As it leaves the Solar System it will be approximately right ascension (RA) 23h51m and declination +24°45′, in Pegasus. It will continue to slow down until it reaches a speed of 26.33 km/s relative to the Sun, the same speed it had before its approach to the Solar System. It will take the object roughly 20,000 years to leave the Solar System completely.

Accounting for Vega’s proper motion, it would have taken ʻOumuamua 600,000 years to reach the Solar System from Vega. But as a nearby star, Vega was not in the same part of the sky at that time. Astronomers calculate that one hundred years ago, the asteroid was 561 AU (83.9 billion km; 52.1 billion mi) from the Sun and traveling at 26.33 km/s with respect to the Sun. This interstellar speed is very close to the mean motion of material in the Milky Way in the neighborhood of the Sun, also known as the local standard of rest (LSR), and especially close to the mean motion of a relatively close group of M dwarf stars. This velocity profile also indicates an extrasolar origin, but appears to rule out the closest dozen of stars. In fact, the strong correlation between ʻOumuamua’s velocity and the local standard of rest, might mean that it has circulated the galaxy several times and thus may have originated from an entirely different part of the Milky Way.

It is unknown how long the object has been traveling among the stars. The Solar System is likely the first star system that ʻOumuamua has closely encountered since being ejected from its birth star system, potentially several billion years ago. It has been speculated that the object may have been ejected from a stellar system in one of the local kinematic associations of young stars (Carina or Columba specifically), within a range of about 100 parsecs, some 45 million years ago. The Carina and Columba associations are now very far in the sky from the Lyra constellation, the direction from which ʻOumuamua came when it entered the Solar System. Others have speculated that it was ejected from a white dwarf system and that its volatiles were lost when its star became a red giant. About 1.3 million years ago the object may have passed within a distance of 0.16 parsecs (0.52 light-years) to the nearby star TYC 4742-1027-1, but its velocity is too high to have originated from that star system, and it probably just passed through the system’s Oort cloud at a speed of 103 km/s (230,000 mph).

According to one hypothesis, ʻOumuamua could be a fragment from a tidally disrupted planet.

Source : Wikipedia

If you want to view Oumuamua’s position in WinStars, please download the latest version of the program (3.0.22 beta) and activate the Oumuamua module .

GW150914 : first observation of gravitational waves

The first observation of gravitational waves was made on 14 September 2015 and was announced by the LIGO and Virgo collaborations on 11 February 2016. Previously gravitational waves had only been inferred indirectly, via their effect on the timing of pulsars in binary star systems.

The waveform, detected by both LIGO observatories, matched the predictions of general relativity for a gravitational wave emanating from the inward spiral and merger of a pair of black holes of around 36 and 29 solar masses and the subsequent “ringdown” of the single resulting black hole. The signal was named GW150914 (from “Gravitational Wave” and the date of observation 20150914).


The Laser Interferometer Gravitational-Wave Observatory

It was also the first observation of a binary black hole merger, demonstrating both the existence of binary stellar-mass black hole systems, and the fact that such mergers could occur within the current age of the universe.

This first observation was reported around the world as a remarkable accomplishment for many reasons. Efforts to directly prove the existence of such waves had been ongoing for over fifty years, and the waves are so minuscule that Albert Einstein himself doubted that they could ever be detected. The waves given off by the cataclysmic merger of GW150914 reached Earth as a ripple in spacetime that changed the length of a 4-km LIGO arm by a thousandth of the width of a proton, proportionally equivalent to changing the distance to the nearest star outside the Solar System by one hair’s width. The energy released by the binary as it spiralled together and merged was immense, with the energy of 3.0 c2 solar masses (5.3×1047 joules or 5300 foes) in total radiated as gravitational waves, reaching a peak emission rate of about 3.6×1049 watts – a level greater than the combined power of all light radiated by all the stars in the observable universe.


The gravitational-wave event GW150914 observed by the LIGO Hanford

The observation confirms the last remaining unproven prediction of general relativity and validates its predictions of space-time distortion in the context of large scale cosmic events (known as strong field tests). It was also heralded as inaugurating a new era of gravitational-wave astronomy, which will enable observations of violent astrophysical events that were not previously possible, and potentially allow the direct observation of the very earliest history of the universe.

Albert Einstein originally predicted the existence of gravitational waves in 1916, on the basis of his theory of general relativity. General relativity interprets gravity as a consequence of distortions in space-time, caused by mass. Therefore, Einstein also predicted that events in the cosmos would cause “ripples” in space-time – distortions of space-time itself – which would spread outward, although they would be so minuscule that they would be nearly impossible to detect by any technology foreseen at that time. It was also predicted that objects moving in an orbit would lose energy for this reason (a consequence of the law of conservation of energy), as some energy would be given off as gravitational waves, although this would be insignificantly small in all but the most extreme cases.


Location of the detection signal GW150914 in WinStars (activate the Ligo module)

One case where gravitational waves would be strongest is during the final moments of the merger of two compact objects such as neutron stars or black holes. Over a span of millions of years, binary neutron stars, and binary black holes lose energy, largely through gravitational waves, and as a result, they spiral in towards each other. At the very end of this process, the two objects will reach extreme velocities, and in the final fraction of a second of their merger a substantial amount of their mass would theoretically be converted into gravitational energy, and travel outward as gravitational waves, allowing a greater than usual chance for detection. However, since little was known about the number of compact binaries in the universe and reaching that final stage can be very slow, there was little certainty as to how often such events might happen.

Direct observation of gravitational waves was not possible for the many decades after they were predicted due to the minuscule effect that would need to be detected and separated from the background of vibrations present everywhere on Earth. A technique called interferometry was suggested in the 1960s and eventually technology developed sufficiently for this technique to become feasible.

In the present approach used by LIGO, a laser beam is split and the two halves are recombined after travelling different paths. Changes to the length of the paths or the time taken for the two split beams, caused by the effect of passing gravitational waves, to reach the point where they recombine are revealed as “beats”. Such a technique is extremely sensitive to tiny changes in the distance or time taken to traverse the two paths. In theory, an interferometer with arms about 4 km long would be capable of revealing the change of space-time – a tiny fraction of the size of a single proton – as a gravitational wave of sufficient strength passed through Earth from elsewhere. This effect would be perceptible only to other interferometers of a similar size, such as the Virgo, GEO 600 and planned KAGRA and INDIGO detectors. In practice at least two interferometers would be needed, because any gravitational wave would be detected at both of these but other kinds of disturbance would generally not be present at both, allowing the sought-after signal to be distinguished from noise. This project was eventually founded in 1992 as the Laser Interferometer Gravitational-Wave Observatory (LIGO). The original instruments were upgraded between 2010 and 2015 (to Advanced LIGO), giving an increase of around 10 times their original sensitivity.

LIGO operates two gravitational-wave observatories in unison, located 3,002 km (1,865 mi) apart: the LIGO Livingston Observatory in Livingston, Louisiana, and the LIGO Hanford Observatory, on the DOE Hanford Site near Richland, Washington. The tiny shifts in the length of their arms are continually compared and significant patterns which appear to arise synchronously are followed up to determine whether a gravitational wave may have been detected or if some other cause was responsible.

Initial LIGO operations between 2002 and 2010 did not detect any statistically significant events that could be confirmed as gravitational waves. This was followed by a multi-year shut-down while the detectors were replaced by much improved “Advanced LIGO” versions.  In February 2015, the two advanced detectors were brought into engineering mode, with formal science observations due to begin on 18 September 2015.

Throughout the development and initial observations by LIGO, several “blind injections” of fake gravitational wave signals were introduced to test the ability of the researchers to identify such signals. To protect the efficacy of blind injections, only four LIGO scientists knew when such injections occurred, and that information was revealed only after a signal had been thoroughly analyzed by researchers. No such tests took place in September 2015, when GW150914 was detected.

GW150914 was detected by the LIGO detectors in Hanford, Washington state, and Livingston, Louisiana, USA, at 09:50:45 UTC on 14 September 2015. The LIGO detectors were operating in “engineering mode”, meaning that they were operating fully but had not yet begun a formal “research” phase (which was due to commence three days later on 18 September), so initially there was a question as to whether the signals had been real detections or simulated data for testing purposes before it was ascertained that they were not tests.

The chirp signal lasted over 0.2 seconds, and increased in frequency and amplitude in about 8 cycles from 35 Hz to 250 Hz. The signal is in the audible range and has been described as resembling the “chirp” of a bird; astrophysicists and other interested parties the world over excitedly responded by imitating the signal on social media upon the announcement of the discovery. (The frequency increases because each orbit is noticeably faster than the one before during the final moments before merging.)

The trigger that indicated a possible detection was reported within three minutes of acquisition of the signal, using rapid (‘online’) search methods that provide a quick, initial analysis of the data from the detectors. After the initial automatic alert at 09:54 UTC, a sequence of internal emails confirmed that no scheduled or unscheduled injections had been made, and that the data looked clean. After this, the rest of the collaborating team was quickly made aware of the tentative detection and its parameters.

More detailed statistical analysis of the signal, and of 16 days of surrounding data from 12 September to 20 October 2015, identified GW150914 as a real event, with a significance estimated by one analysis of 6.7 sigma and a significance bound estimated by another analysis of at least 5.1 sigma or a confidence level of 99.99994%. Corresponding wave peaks were seen at Livingston seven milliseconds before they arrived at Hanford. Gravitational waves propagate at the speed of light, and the disparity is consistent with the light travel time between the two sites. The waves had traveled at the speed of light for more than a billion years.

At the time of the event, the Virgo gravitational wave detector (near Pisa, Italy) was offline and undergoing an upgrade; had it been online it would likely have been sensitive enough to also detect the signal, which would have greatly improved the positioning of the event. GEO600 (near Hannover, Germany) was not sensitive enough to detect the signal. Consequently, neither of those detectors was able to confirm the signal measured by the LIGO detectors.

The event happened at a luminosity distance of 440 megaparsecs (determined by the amplitude of the signal), or 1.4 billion light years, corresponding to a cosmological redshift of 0.093 (90% credible intervals). Analysis of the signal along with the inferred redshift suggested that it was produced by the merger of two black holes with masses of 35 times and 30 times the mass of the Sun (in the source frame), resulting in a post-merger black hole of 62 solar masses. The mass–energy of the missing 3.0 solar masses was radiated away in the form of gravitational waves.

During the final 20 milliseconds of the merger, the power of the radiated gravitational waves peaked at about 3.6×1049 watts – 50 times greater than the combined power of all light radiated by all the stars in the observable universe.

Across the 0.2-second duration of the detectable signal, the relative tangential (orbiting) velocity of the black holes increased from 30% to 60% of the speed of light. The orbital frequency of 75 Hz (half the gravitational wave frequency) means that the objects were orbiting each other at a distance of only 350 km by the time they merged. The phase changes to the signal’s polarization allowed calculation of the objects’ orbital frequency, and taken together with the amplitude and pattern of the signal, allowed calculation of their masses and therefore their extreme final velocities and orbital separation (distance apart) when they merged. That information showed that the objects had to be black holes, as any other kind of known objects with these masses would have been physically larger and therefore merged before that point, or would not have reached such velocities in such a small orbit. The highest observed neutron star mass is two solar masses, with a conservative upper limit for the mass of a stable neutron star of three solar masses, so that a pair of neutron stars would not have had sufficient mass to account for the merger (unless exotic alternatives exist, for example, boson stars), while a black hole-neutron star pair would have merged sooner, resulting in a final orbital frequency that was not so high.

The decay of the waveform after it peaked was consistent with the damped oscillations of a black hole as it relaxed to a final merged configuration. Although the inspiral motion of compact binaries can be described well from post-Newtonian calculations, the strong gravitational field merger stage can only be solved in full generality by large-scale numerical relativity simulations.

The post-merger object is thought to be a rotating Kerr black hole with a spin parameter of 0.68, i.e. one with 2/3 of the maximum possible angular momentum for its mass.

The two stars which formed the two black holes were likely formed about 2 billion years after the Big Bang with masses of between 40 and 100 times the mass of the Sun.

Gravitational wave instruments are whole-sky monitors with little ability to spatially resolve signals. A network of such instruments is needed to locate the source in the sky through triangulation. With only the two LIGO instruments in observational mode, GW150914’s source location could only be confined to an arc on the sky. This was done via analysis of the 6.9 ms time-delay, along with amplitude and phase consistency across both detectors. This analysis produced a credible region of 150 deg2 with a probability of 50% or 610 deg2 with a probability of 90% located mainly in the Southern Celestial Hemisphere, in the rough direction of (but much farther than) the Magellanic Clouds.

For comparison, the area of the constellation Orion is 594 deg2.

The announcement of the detection was made on 11 February 2016 at a news conference in Washington, D.C. by David Reitze, the executive director of LIGO, with a panel comprising Gabriela González, Rainer Weiss and Kip Thorne, of LIGO, and France A. Córdova, the director of NSF. Barry Barish delivered the first presentation on this discovery to a scientific audience simultaneously with the public announcement.

The initial announcement paper was published during the news conference in Physical Review Letters, with further papers either published shortly afterwards or immediately available in preprint form.

In May 2016, the full collaboration, and in particular Ronald Drever, Kip Thorne, and Rainer Weiss, received the Special Breakthrough Prize in Fundamental Physics for the observation of gravitational waves. Drever, Thorne, Weiss, and the LIGO discovery team also received the Gruber Prize in Cosmology. Drever, Thorne, and Weiss were also awarded the 2016 Shaw Prize in Astronomy and the 2016 Kavli Prize in Astrophysics. Barish was awarded the 2016 Enrico Fermi Prize from the Italian Physical Society (Società Italiana di Fisica). In January 2017, LIGO spokesperson Gabriela González and the LIGO team were awarded the 2017 Bruno Rossi Prize.

The 2017 Nobel Prize in Physics was awarded to Rainer Weiss, Barry Barish and Kip Thorne “for decisive contributions to the LIGO detector and the observation of gravitational waves”.

 

Source: wikipedia

In order to go further :

  • The initial announcement paper published in Physical Review Letter : https://journals.aps.org/prl/pdf/10.1103/PhysRevLett.116.061102
  • Gravitation et Cosmologie, S. Weinberg
  • General Relativity – An introduction for Physicists, M.P. Hobson, G.P.  Efstathiou et A.N. Lasenby
  • Basic Relativity, R. Mould
  • Relativity – Special, General and Cosmological, W. Rindler
  • Gravitation, C.W. Misner, K.S. Thorne et J.A. Wheeler

 

An all-sky picture by Serge brunier

During the International Year of Astronomy 2009, and in collaboration with the European Southern Observatory, the Milky way was photographed by Serge Brunier mainly from the European observatory sites under the pristine sky of Atacama Desert of Chile (in the southern hemisphere) and La Palma observatory in the Canary Islands (in the northern hemisphere). The all-sky image is in fact a mosaic composed of almost 300 fields, each captured four times, for a total of 1200 photos. All were taken with a Nikon D3 digital camera and a 50 mm lens at f5.6. Each image is the result of a 6-minute exposure. The apparent motion of the sky, caused by Earth’s rotation, was corrected using a small equatorial tracking mount.

As noted by the french photographer and astronomy writer “I started imaging in summer 2008 in Chile from the La Silla Observatory, and then from the Cerro Paranal Observatory, home to the most famous Very Large Telescope array. In addition to pristine skies, in the Atacama Desert I had the opportunity to enjoy exceptional meteorological conditions, as the sky is clear almost eleven months per year.”

With the author’s permission, it’s possible to display this mosaic in WinStars by checking the option “Brunier” which appears in the module part of the configuration box.

p>

source : http://www.twanight.org/newTWAN/news.asp?newsID=6037

 

 

3.0.8 alpha is now available

In this version, a huge memory leak has been fixed in the menu system. The new texture of Pluto is coming from New Horizons data, based on the  published Pluto map by NASA.

With this revision, WinStars 3 can run now on macOS and Ubuntu based OS.

 

The alpha release for Windows and Android is available for testing !

Hi !

The first Alpha release of WinStars 3.0 is now available for testing.

You can find the android package by searching for “WinStars lite” in the Google Play store. Before taking part in the tests, it is necessary to send an empty message to alpha-en-join@vps254960.ovh.net 

The installer for Windows is available at the following address : https://winstars.net/files/version3/winstars_installer.exe

What is an Alpha test?
Alpha stage software is generally functional but many features are either missing or incomplete. The focus of alpha testing is on reducing or eliminating bugs before the application is released publicly, and often involves hands-on testing by selected end-users.