Binary Stars

The measured characteristics of binary pulsars provide valuable insights into the evolution of these systems. We study the aspects of binary evolution particularly relevant to binary Millisecond Pulsars (MSPs), and the formation of close binaries involving degenerate stars through a spin-evolution diagram (spin-up line). For this task, we use a wide variety of binaries, including those with compact components that observed in different energy bands, which we analyze them according to the spin-up line. Their formation and evolution over timescales of binary evolution models are investigated in order to grab any constraint on their evolution, and to estimate the masses of neutron stars with different mass-transfer histories.

The emergence of intelligence is likely a relatively recent phenomena throughout the cosmos. The total number of habitable extraterrestrial planets within the Milky Way capable of supporting advanced, intelligent life within the next 500 Myr is <5,162. Almost all of which are earth-like orbiting around a single star with mass ranges from 0.628 to 1 solar mass. No exomoons are capable of supporting advanced life, and a negligible number of low mass binary systems (<0.628 solar mass) are habitable. The nearest extraterrestrial industrial civilization lies at least 88.7 million light years away, and possibly 111 million light years beyond. No extraterrestrial civilization arises before 232.74 Mya within the observable universe, and no extraterrestrial civilization arises before 270.95 Mya within the universe by co-moving distance. Despite great distances between the nearest civilizations and the low probability of emergence within our vicinity, given the sheer size of the univers...

The Search for Extra-Terrestrial Intelligence (SETI) has so far been unsuccessful and demands additional methods. To achieve this, we introduce a two-dimensional metric for civilizational development, using the Kardashev scale of energy use and the Barrow scale of inward manipulation. We advance energetic, societal, scientific, computational, and philosophical arguments that black holes are attractors for intelligence. An application of the two-dimensional metric leads to a simple, consistent and observable hypothesis to test the existence of very advanced civilizations. We suggest that some already observed X-Ray Binaries may be unnoticed advanced civilizations, scoring high on both the Kardashev and Barrow scales. The appendix provides an argumentative map of the paper's main thesis.

Keywords: SETI, black holes, Kardashev scale, Barrow scale, star lifting, XRB

Correction: This statement "Freeman Dyson proposed in his landmark (1979) paper that a civilization could [...] exploit the time dilation effects generated by black holes to survive forever" is wrong, his argument had not to do with dilation effects.

More info: Vidal, C. 2011 Black Holes: Attractors for Intelligence? Kavli Royal Society International Centre, "Towards a scientific and societal agenda on extra-terrestrial life", 4-5 Oct 2010.http://arxiv.org/abs/1104.4362 http://student.vub.ac.be/~clvidal/writings/Vidal-Black-Holes-Intelligence.pdf

More fascinating open questions at: http://evodevouniverse.com/wiki/Research_on_SETI,_black_holes,_XRB_and_star_lifting

News report at: http://news.discovery.com/space/super-civilizations-might-live-off-black-holes-110430.html

Arundhati, the icon of Chastity who never crossed the path of her husband Vasishtha is identified with the star Alcor, closely following the star Mizar, her binary companion, in the constellation of Ursa Major. An appearance contrary to this was reported by Vyasa as a 'Nimitta' sometime before the starting of the Mahabharata war. Why it was a nimitta and why that appearance was transient that could not have lasted for 6000 years as claimed by Mr.Nilesh Oak to date Mahabharata war, is originally explained in the 9th chapter of my book "MYTH OF ‘THE EPOCH OF ARUNDHATI’ OF NILESH NILKANTH OAK" critiquing his date. That chapter is reproduced here to enable readers to know why Mr Oak is wrong and why the observation by Vyasa was only a nimitta.

The emergence of intelligence is a relatively recent phenomena throughout the cosmos. The total number of habitable extraterrestrial planets within the Milky Way capable of supporting advanced, intelligent life within the next 500 Myr is <969. Most of which are earth-like orbiting around a single star with mass ranges from 0.712 to 1 solar mass. No exomoons are capable of supporting advanced life, and a negligible number of low mass binary systems (<0.712 solar mass) are habitable. The nearest extraterrestrial industrial civilization lies at least 51.85 million light years away, and possibly at least 100 million light years or beyond. No extraterrestrial civilization arises before 119 Mya within the observable universe, and no extraterrestrial civilization arises before 138 Mya within the universe by co-moving distance. Despite great distances between the nearest civilizations and the low probability of emergence within our vicinity, given the sheer size of the universe, the total number of intelligent extraterrestrial civilizations likely approaches infinity or \left(\frac{1}{4.4\cdot10^{7}}\right)^{3}\cdot3.621\cdot10^{6}\cdot10^{10^{10^{122}}} if the universe is finitely bounded. Based on incentives for economic growth, all civilizations tend to expands near the speed of light and will eventually universally connect with each other via wormhole networks. Within such a network, the farthermost distances traversable from earth can be either infinite or 3.621\cdot10^{6}\cdot10^{10^{10^{122}}}light years in radius if the universe is finitely bounded...

The emergence of intelligence is a relatively recent phenomena throughout the cosmos. The total number of habitable extraterrestrial planets within the Milky Way capable of supporting advanced, intelligent life within the next 500 Myr is &lt;10,799. Almost all of which are earth-like orbiting around a single star with mass ranges from 0.628 to 1 solar mass. No exomoons are capable of supporting advanced life, and a negligible number of low mass binary systems (&lt;0.628 solar mass) are habitable. The nearest extraterrestrial industrial civilization lies at least 88.7 million light years away, and possibly 111 million light years beyond. No extraterrestrial civilization arises before 232.74 Mya within the observable universe, and no extraterrestrial civilization arises before 270.95 Mya within the universe by co-moving distance. Despite great distances between the nearest civilizations and the low probability of emergence within our vicinity, given the sheer size of the universe, the...

In September 2016, Gaia DR1 was released. Positions, parallaxes, and proper motions, for 2 milions of stars (mag.< +11.5) , in common between the Tycho-2 Catalogue and Gaia, is contained in Gaia Data Release 1. This part of Gaia DR1 is based on the Tycho-Gaia Astrometric Solution (TGAS).
The parallax and proper motion published in this first data release have been used to review the distance of the double star identified in the Washington Double Star Catalog as 04053+2348 MCN 1 studied by the author in January, 2016. Also, are shown the data about the photometry, temperature, spectral class, mass of both components using a mathematical model of evolutionary stellar traces and isochrones.
This work was published in the italian quarterly magazine “Bulletin of Double Stars” (ISSN 2279-9044 Bibcode: BolSD)  number 22, July - September 2017, pp04-13 on the website: https://sites.google.com/site/ilbollettinodellestelledoppie/archivio---archive
The Washington Double Star Catalog (WDS) maintained by the United States Naval Observatory (USNO) is the world's principal database of astrometric double and multiple star information. The WDS Catalog contains positions (J2000), discoverer designations, epochs, position angles, separations, magnitudes, spectral types, proper motions, and, when available, Durchmusterung numbers and notes for the components of 141,842  systems based on 1,585,539 means. Of these, 23,862 are physical, 4,988 are optical, and 112,992 are unknown. The current version is updated nightly.
It’s available at URL :
http://www.usno.navy.mil/USNO/astrometry/optical-IR-prod/wds/WDS

Average case complexity, in order to be a useful and reliable measure, has to be robust. The probability distribution, generally uniform, over which expectation is taken should be realistic over the problem domain. But algorithm books do not certify that the uniform inputs are always realistic. Do the results hold even for non uniform inputs? In this context we observe that Binary Tree sort is more robust than the fast and popular Quick sort in the average case.

Possibly the only online video and online simulation available anywhere, of the orbit of this planet whose possible existence was first proposed by Ramm et al (2009).  If it exists, it would be the first discovery ever of a planet with a backwards orbit around one star of a binary star system.

The Washington Double Stars Catalog (WDS) is, undoubtedly,
the Bible of the double stars. It is based on other many catalogues and on observations of many different astronomers. It  is not of surprising, therefore, that some of the stars listed in it are duplicated

This article intends to fathom a development by M.Tailherer which introduces a second gravitational equation devised to complete General Relativity (TGR), based on the ansatz of equating the curvature tensor opportunely contracted to the 4-vorticity by a new constant S as measure of the intrinsic inertia of the curved Space-Time. After justifying the need to deal with the 2nd fundamental tensor in Relativity in discussing the dynamics of Space-Time structure, it has been shown how the model exhibits unforeseen analogies with the electromagnetic theory. As direct continuation of the analysis of the gravitational wave propagation in free space, it has been seen that on asymptotic conditions the polarization state can be retrieved as mixture of two independent modes likewise TGR as from harmonic constraints on the homogeneous solution of wave equation. Actually, in this gravitational framework, at least for one polarization state, transverse waves propagate causing equal in-phase deformation displacement, not counter-phase as expected in gravitational interferometry experiments at present status. Computation of gravitational power losses for the keplerian system B 1913+16 in the solution by approximations of the inhomogeneous problem has been carried out to the 1st order, which has allowed the attempt of the assessment of a new universal gravitational constant for the first time ever.

A revised orbit, with period of 1505 yr, and system mass, 3.65 AE 0.60 M , are presented for the visual binary WDS 23186+6807AB. The total mass is well in accord with estimates from the literature made on the basis of different methods. The G8 III spectral type of the primary is confirmed. Key words: astrometry — binaries: visual — stars: individual (WDS 23186+6807AB = HD 219916)

HW Vir systems are rare evolved eclipsing binaries composed of a hot compact star and a low-mass main sequence star in a close orbit. These systems provide a direct way to measure the fundamental properties, e.g. masses and radii, of their components, hence they are crucial in studying the formation of subdwarf B stars and low-mass white dwarfs, the common-envelope phase and the pre-phase of cataclysmic variables. Here, we present a detailed study of HS 2231+2441, an HW Vir type system, by analysing BVR C I C photometry and phase-resolved optical spectroscopy. The spectra of this system, which are dominated by the primary component features, were fitted using non-local thermodynamic equilibrium models providing an effective temperature T eff = 28 500 ± 500 K, surface gravity log g = 5.40 ± 0.05 cm s −2 and helium abundance log (n(He)/n(H)) = −2.52 ± 0.07. The geometrical orbit and physical parameters were derived by simultaneously modelling the photometric and spectroscopic data using the Wilson–Devinney code. We derive two possible solutions for HS 2231+2441 that provide the component masses: M 1 = 0.19 M and M 2 = 0.036 M or M 1 = 0.288 M and M 2 = 0.046 M. Considering the possible evolutionary channels for forming a compact hot star, the primary of HS 2231+2441 probably evolved through the red-giant branch scenario and does not have a helium-burning core, which is consistent with a low-mass white dwarf. Both solutions are consistent with a brown dwarf as the secondary.

A binary star is a system that contains two stars orbiting about a common
centre of mass. This report aims in determining the orbital period and the
masses of the binary star in the binary system WW Cnc using photometry
method.
Telescopic images of WW Cnc were obtained daily for a period of about three
weeks. The images obtained were uncompressed and transformed for easy
analysis (using softwares-DS9, IRIS, WEBHERA). Photometry
measurements were done using IRIS- this involved both aperture photometry
and automatic photometry.
Magnitudes of WW Cnc were obtained which were used to plot a light curve.
The light curve obtained was used to calculate the orbital period of WW Cnc.
The results obtained were also used to calculate the mass of WW Cnc using
the magnitude-luminosity relation.
The results obtained were in line with the already known values.

This paper describes the astrometric study of a new pair of stars in Taurus constellation. The primary star of this pair is 2MASS J04051537+2347501. Are shown the data about the kinematics, photometry, distance, spectral class, mass of both components and the relative astrometry using the plates of the Palomar Observatory Sky Survey (POSSI and POSSII) of different epochs and one image of the author. This study was published in the italian quarterly magazine “Bulletin of Double Star” (ISSN 2279-9044 Bibcode: BolSD) in the Vol.16, January - March 2016, pagg.26-33 on the website : https://sites.google.com/site/ilbollettinodellestelledoppie/archivio---archive This research has contributed to include in the “Washington Visual Double Star Catalog” (Brian D. Mason, Gary L. Wycoff, and William I. Hartkopf , 2001-2015 edition) the discovery of a new pair of stars. The WDS Identifier is : 04053+2348 MCN 1 The Washington Double Star Catalog (WDS), maintained by the United States Naval Observatory (USNO), is the world's principal database of astrometric double and multiple star information. The WDS Catalog contains positions (J2000), discoverer designations, epochs, position angles, separations, magnitudes, spectral types, proper motions, and, when available, Durchmusterung numbers and notes for the components of 115,769 systems based on 824,698 means (as of 1 January 2012). It’s available at URL : http://www.usno.navy.mil/USNO/astrometry/optical-IR prod/wds/WDS

The recently reported gravitational wave events GW150914 and GW151226 caused by the merg- ers of binary black holes [1–3] provide a formidable way to set constraints on alternative metric theories of gravity in the strong field regime. In this paper, we develop an approach where an arbitrary theory of gravity can be parametrised by an effective coupling Geff and an effective grav- itational potential Φ(r). The standard Newtonian limit of General Relativity is recovered as soon as Geff → GN and Φ(r) → ΦN. The upper bound on the graviton mass and the gravitational interaction length, reported by the LIGO-VIRGO collaboration, can be directly recast in terms of the parameters of the theory which allows an analysis where the gravitational wave frequency modulation sets constraints on the range of possible alternative models of gravity. Numerical results based on published parameters for the binary black hole mergers are also reported. Comparison of the observed phase of the GW150914 and GW151226 with the modulated phase in alternative theories of gravity does not give reasonable constraints due the large uncertainties in the estimated parameters for the coalescing black holes. In addition to these general considerations, we obtain limits for the frequency dependence of the α parameter in scalar tensor theories of gravity.

I am reporting on observations and analysis of a probable, new delta Scuti variable star, GSC 02087-02155, which was discovered in a data run of the STExTS project exoplanet search during a seven-week period the summer of 2012 in Pitkin, Colorado. R-band observations were made with a 200 mm astrograph f/1.5 stopped down to f/2.8. Over 10,500 images were processed in a data pipeline and light curves were analyzed with Peranso software. The candidate star has a magnitude of 9.36 and an observed pulsation amplitude of 0.060 mag with a fundamental period of 0.0910(2) day as well as possibly exhibiting the Blazhko Effect. The observations and analysis of the star as well as preliminary modeling are presented.

This paper presents new common proper-motion binaries detected by applying well-known statistical criteria over large subsets of the astrometric catalogs available online. All the pairs have been confirmed by checking the photographic plates and are not included in the Washington Double Star Catalog. An initial measurement of separation and
position angle has been obtained for each pair.

The study of eclipsing binary stars is a key area of interest in astrophysics, that helps determining a multitude of astronomical properties, from stellar evolution to stellar classification to the relative locations of astronomical objects and the structure of the galaxy itself. This project utilises photometric data in the near-Infrared spectrum to describe a method of determing properties such as Temperature, distances and stellar classification from photometric data. Due to the limitations of infrared data, the results for the stellar type distribution and properties were different from what was expected. A more extensive study with optical data would be able to utilise the method to determine various properties of stars in eclipsing binary systems with a higher degree of accuracy. Declaration I declare that this project and report is my own work.

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We present a new BVR light curves of the system EQ Tau carried out in the period from March to April 2006 using a 50-cm F/8.4 Ritchey–Chretien telescope (Ba50) of the Baja Astronomical Observatory (Hungary), and 512 × 512 Apogee AP-7 CCD camera. The observed light curves were analyzed using the 2004 version of the Wilson-Devinney code. The results show that the more massive component is hotter than the low massive one by 100 K. A long term orbital period study shows that the period increases by the rate 8.946 (±0.365) x10-11 days/cycle. Evolutionary state of the system has been investigated and showed that, the primary component of the system is located nearly on the ZAMS for both the M-L and M-R relations. The secondary component is close to the TAMS track for M-L and above the M-R relations.