N. KAMESWARA RAO
Articles written in Journal of Astrophysics and Astronomy
Volume 3 Issue 1 March 1982 pp 79-92
Ultraviolet observations of the hydrogen-deficient variable star MV sagittarii
IUE observations of the hydrogen-deficient irregular variable star MV Sgr obtained in 1980 June-October and also in 1979 November are discussed. These observations show a prominent λ 2200 absorption feature. A value of
Volume 3 Issue 3 September 1982 pp 267-276
HD 147010: The Ap star in the reflection nebula vdB 102 in upper Scorpius region
HD 147010, which is in the reflection nebula vd B 102, has been found to be a hot Ap silicon star rather than a normal A supergiant. From the
Volume 4 Issue 1 March 1983 pp 59-63
Ultraviolet variability of HD 62001 – The central star of the missing nebula V-V 1-7
IUE observations of HD 62001 do not confirm the ultraviolet variability of 0.15 mag seen from the ANS observations. These intriguing variations in ANS observations seem to be caused by a nearby (∼ 70 arcsec away) B star getting in and out of the field of view of the telescope, which had a jitter of 20 arcsec. There seems to be no evidence for the presence of a hot companion, either from the energy distribution or from UV variability. However, visual light variations are present. This, coupled with the radial velocity variations, indicates a binary nature probably of Algol type.
Volume 6 Issue 2 June 1985 pp 101-112
Observations of hydrogen deficient binary Upsilon sagittarii
N. Kameswara Rao V. R. Venugopal
The absolute magnitude
Volume 6 Issue 3 September 1985 pp 153-157
VLA observations of extreme hydrogen deficient stars
N. Kameswara Rao V. R. Venugopal A. Patnaik
VLA observations at 2 and 6 cm have been obtained for six hydrogen-deficient stars R CrB, HD 160641, BD — 9°4395, V348 Sgr, MV Sgr and Sgr
Volume 8 Issue 2 June 1987 pp 195-209
Evolution of the optical spectrum of SN 1987a in the large magellanic cloud
B. N. Ashoka G. C. Anupama T. P. Prabhu S. Giridhar K. K. Ghosh S. K. Jain A. K. Pati N. Kameswara Rao
The evolution of the spectrum of SN1987a is traced from 1987 February 26 to March 31. Based on the low-resolution spectroscopic data we identify the lines of H, He I, Na I, Fe II, Sc II, Ca II which are known to be present in Type II Supernovae, and also present evidence for the existence of lines of Mg I, CaI, O I, and N I. We discuss the evolution of the Hα profile, and draw attention to its complex structure around March 30. Close to the rest wavelength of Ha a double-peaked structure appeared in the profile with a peak-to-peak separation of ∼ 1400 km s−1, suggestive of an expanding shell or disc of gas.
Using the available broadband photometric information, we also trace the evolution of the photosphere of SN1987a assuming that it radiates like a supergiant.
Volume 8 Issue 3 September 1987 pp 227-230
Further VLA observations of hydrogen deficient stars
N. Kameswara Rao V. R. Venugopal A. R. Patnaik
VLA observations at 6 cm have been obtained for three hydrogen-deficient objects υ Sgr, V 348 Sgr, and A bell 58. A bell 58 was also observed at 2 cm. Only upper limits to the flux density could be set for these sources. A new radio source at 6 cm was found in the field of υ Sgr.
The upper limit for 6 cm flux density of V348 Sgr sets an upper limit to its reddening as
Volume 11 Issue 1 March 1990 pp 37-42
Emission spectrum of hot R OB star MV Sgr
N. Kameswara Rao L. Houziaux Sunetra Giridhar
The new spectroscopic observation of MV Sgr obtained at ESO in 1987 July shows enhanced emission lines of He I λ3889, [S
Volume 11 Issue 2 June 1990 pp 151-166
CCD photometry in
R. Surendiranath N. Kameswara Rao Ram Sagar J. S. Nathan K. K. Ghosh
The open cluster NGC 2818 containing a planetary nebula has been observed in
Volume 11 Issue 4 December 1990 pp 445-460
The eccentric double-lined binary BD — 1° 1004
N. Kameswara Rao B. N. Ashoka C. Lloyd C. D. Pike D. J. Stickland
A new radial velocity study has been made of the highly eccentric, early-type binary BD -1° 1004 using spectra from the Kavalur Observatory. All available archival material has also been reexamined. An attempt has been made to correct for line ‘dragging’ by the secondary spectrum to improve the fit of the observed data to the orbital solutions. It is found that an earlier suggestion of apsidal regression is still possible although ω is probably constant within the errors. There remain problems and inconsistencies with other orbital elements, in particular K1 and γ
Volume 11 Issue 4 December 1990 pp 475-490
High resolution spectroscopy of R Coronae Borealis during the 1988— 1989 minimum
David L. Lambert N. Kameswara Rao Sunetra Giridhar
Moderate-resolution spectra of the C2 Swan 0-1 bandhead, the Na I D lines and the KI resonance lines near 7660 Å obtained at minimum light during the 1988–1989 decline of R CrB are discussed and interpreted in terms of a popular model for R CrB declines. High-resolution spectra obtained at maximum light show blue-shifted chromospheric emission in the cores of the Na I D and the Sc π 4246.8 Å lines
Volume 13 Issue 2 June 1992 pp 175-194
Mid-ultraviolet and optical photometry of helium stars
Gopal C. Kilambi Praveen Nagar N. Kameswara Rao
Mid-ultraviolet and optical photometric analysis of helium stars are presented. A linear relation exists between the effective temperature derived from model atmospheres and (1965-V)0 index. The effective temperatures derived from (1965-V)0 index are somewhat higher than that of MK spectral type estimates especially for late B-type helium objects.
Volume 13 Issue 4 December 1992 pp 307-318
High resolution spectroscopy of the semi-regular variable LR Sco
Sunetra Giridhar N. Kameswara Rao David L. Lambert
A detailed spectroscopic investigation of LR Sco which was earlier misclassified as R CrB star is made. Atmospheric parameters and elemental abundances are determined using detailed depth-dependent model atmospheres and line synthesis technique. Most of the elements show near solar abundances.
The strength of circumstellar components seen in Na D lines are used to derive the mass loss rate. Another independent estimate of mass loss rate is made using the observed infrared flux from 1–100Μm. These two approaches lead to nearly the same value of mass loss rate when
Volume 15 Issue 1 March 1994 pp 47-67
The R Coronae Borealis stars — A few mere facts
David L. Lambert N. Kameswara Rao
This review presents a selection of recent highlights of observations of R Coronae Borealis variables. Emphasis is placed on an abundance analysis of a complete sample (18 stars) of the warm galactic RCBs. It is shown that 14 of the 18 have very similar compositions: the iron mass fraction ranges about a factor of 3 around the solar value (assuming C/He = 3%) but abundance ratios X/Fe for elements from Na to Ba show little variation. By contrast, the other 4 stars are deficient in iron but not in Na, Si, S and some other elements. With for example, [Si/Fe] ≃ 2, the quartet is indeed ‘peculiar’. One of the quartet, V854 Cen shows depletions of elements (other than CNO) similar to the depletions seen in interstellar medium corresponding to average log
Volume 17 Issue 1-2 June 1996 pp 23-40
Sunetra Giridhar N. Kameswara Rao David L. Lambert
Two high resolution spectra of the hot RCrB star DY Cen in the red region are compared. The photospheric absorption lines show a radial velocity variation of 12 kms-1 between 1989 July and 1992 May. Emission components to some CII lines present in 1989 are almost entirely absent in 1992. Nebular forbidden lines of [OI], [NII] and [SII] appear unchanged from 1989 to 1992
Volume 26 Issue 2-3 June 2005 pp 331-338
High resolution stellar spectroscopy with VBT echelle spectrometer
N. Kameswara Rao S. Sriram K. Jayakumar F. Gabriel
The optical design and performance of the recently commissioned fiber fed echelle spectrometer of 2.34 meter Vainu Bappu Telescope are described. The use of it for stellar spectroscopic studies is discussed.
Volume 38 Issue 2 June 2017 Article ID 0028 Review Article
In-orbit Performance of UVIT and First Results
S. N. Tandon J. B. Hutchings S. K. Ghosh A. Subramaniam G. Koshy V. Girish P. U. Kamath S. Kathiravan A. Kumar J. P. Lancelot P. K. Mahesh R. Mohan J. Murthy S. Nagabhushana A. K. Pati J. Postma N. Kameswara Rao K. Sankarasubramanian P. Sreekumar S. Sriram C. S. Stalin F. Sutaria Y. H. Sreedhar I. V. Barve C. Mondal S. Sahu
The performance of the ultraviolet telescope (UVIT) on-board AstroSat is reported. The performance in orbit is also compared with estimates made from the calibrations done on the ground. The sensitivity is found to be within ∼15% of the estimates, and the spatial resolution in the NUV is found to exceed significantly the design value of 1.8′′ and it is marginally better in the FUV. Images obtained from UVIT are presented to illustrate the details revealed by the high spatial resolution. The potential of multi-band observations in the ultraviolet with high spatial resolution is illustrated by some results.
Volume 41 All articles Published: 11 December 2020 Article ID 0035
The horizontal branch morphology of the globular cluster NGC 1261 using AstroSat
SHARMILA RANI GAJENDRA PANDEY ANNAPURNI SUBRAMANIAM SNEHALALA SAHU N. KAMESWARA RAO
We present the results obtained from the UV photometry of the globular cluster NGC 1261 using far-UV (FUV) and near-UV (NUV) images acquired with the Ultraviolet Imaging Telescope (UVIT) onboard the AstroSat satellite. We utilized the UVIT data combined with HST, GAIA, and ground-based optical photometric data to construct the different UV colour-magnitude diagrams (CMDs). We detected blue HB (BHB), and two extreme HB (EHB) stars in FUV, whereas full HB, i.e., red HB (RHB), BHB as well as EHB is detected in NUV CMDs. The 2 EHB stars, identified in both NUV and FUV, are confirmedmembers of the cluster. The HB stars form a tight sequence in UV-optical CMDs, which is almost aligned with Padova isochrones. This study sheds light on the significance of UV imaging to probe the HB morphology in GCs.
Volume 42 All articles Published: 26 May 2021 Article ID 0020 PAYLOAD REVIEW
In-orbit performance of UVIT over the past 5 years
S. K. GHOSH P. JOSEPH A. KUMAR J. POSTMA C. S. STALIN A. SUBRAMANIAM S. N. TANDON I. V. BARVE A. DEVARAJ K. GEORGE V. GIRISH J. B. HUTCHINGS P. U. KAMATH S. KATHIRAVAN J. P. LANCELOT D. LEAHY P. K. MAHESH R. MOHAN S. NAGABHUSHANA A. K. PATI N. KAMESWARA RAO K. SANKARASUBRAMANIAN P. SREEKUMAR S. SRIRAM
Over the last 5 years, UVIT has completed observations of more than 500 proposals with $\sim$800 unique pointings. In addition, regular planned monitoring observations have been made and from their analysis various key parameters related to in orbit performance of UVIT have been quantified. The sensitivities of the UV channels have remained steady indicating no effect of potential molecular contamination confirming the adequacy of all the protocols implemented for avoiding contamination. The quality of the PSF through the years confirms adequacy of thermal control measures. The early calibrations obtained during the Performance Verification (PV) phase have been further revised for more subtle effects. These include flat fields and detector distortions with greater precision. The operations of UVIT have also evolved through inorbit experience, e.g. tweaking of operational sequencing, protocol for recovery from bright object detection (BOD) shutdowns, parameters for BOD thresholds, etc. Finally, some effects of charged particle hits on electronics led to optimised strategy for regular resetting. The Near-UV channel was lost in one of suchoperations. All the above in-orbit experiences are presented here.
Volume 42 All articles Published: 3 July 2021 Article ID 0071 SCIENCE RESULTS
Planetary nebulae with UVIT: A progress report
N. KAMESWARA RAO F. SUTARIA J. MURTHY A. RAY G. PANDEY
The spectral region between 1250–3000 Å contains important spectral lines to understand the morphological structures and evolution of planetary nebulae. This is the region sampled by UVIT through various filter bands both in the continuum and in emission lines (e.g.. [C
Volume 44, 2023
Continuous Article Publishing mode
Since January 2016, the Journal of Astrophysics and Astronomy has moved to Continuous Article Publishing (CAP) mode. This means that each accepted article is being published immediately online with DOI and article citation ID with starting page number 1. Articles are also visible in Web of Science immediately. All these have helped shorten the publication time and have improved the visibility of the articles.
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