排序方式： 共有14条查询结果，搜索用时 31 毫秒
1.
P. Sriramachandran S. P. Bagare N. Rajamanickam K. Balachandrakumar 《Solar physics》2008,252(2):267-281
High-resolution Fourier Transform Spectrometer sunspot umbral spectra of the National Solar Observatory/National Optical Astronomy
Observatory at Kitt Peak were used to detect rotational lines from 19 electronic transition bands of the molecules LaO, ScO
and VO, in the wavenumber range of 11 775 to 20 600 cm−1. The presence of lines from the following transitions is confirmed: A
2
Π
r1/2 – X
2
Σ
+(0, 0; 0, 1), A
2
Π
r3/2 – X
2
Σ
+(1, 0), B
2
Σ
+ – X
2
Σ
+(0, 0; 0, 1; 1, 0) and C
2
Π
r1/2 – A′2Δ
r3/2(0, 0; 1, 1) of LaO; A
2
Π
r3/2 – X
2
Σ
+(0, 0), A
2
Π
r1/2 – X
2
Σ
+(0, 0) and B
2
Σ
+ – X
2
Σ
+(0, 0) of ScO; and C
4
Σ
− – X
4
Σ
−(0, 1; 1, 0; 0, 2) and (2, 0) of VO. However, the presence of A
2
Π
r3/2 – X
2
Σ
+(0, 0) and C
2
Π
r3/2 – A′2Δ
r5/2(0, 0; 1, 1) of LaO and C
4
Σ
− – X
4
Σ
−(0, 0) of VO are found to be doubtful because the lines are very weak, and detections are difficult owing to heavy blending
by strong rotational lines of other molecules. Equivalent widths are measured for well-resolved lines and, thereby, the effective
rotational temperatures are estimated for the systems for which the presence is confirmed. 相似文献
2.
K. R. Sivaraman M. Jayachandran K. K. Scaria G. S. D. Babu S. P. Bagare A. P. Jayarajan 《Journal of Astrophysics and Astronomy》1984,5(2):149-158
During the eclipse of 1980 February 16 we photographed the solar corona at an effective wavelength of 6300 å. Using a quadruple camera we also obtained the coronal pictures in polarized light for four Polaroid orientations. We have used these observations to derive the coronal brightness and polarization and from these the electron densities in the corona out to a distance of about 2.5 R⊙ from the centre of the disc. The coronal brightness matches well with that of the corona of 1958 October 12. 相似文献
3.
N. Prithivikumaran M. Fernandez Gomez J.J. Lopez Gonzalez S.P. Bagare N. Rajamanickam 《Astrophysics and Space Science》2002,280(4):319-324
The Franck-Condon (FC) factors (transition probabilities) and r-centroids have been evaluated by the reliable numerical integration procedure for the bands of the A
3 φ4 →X
3 φ4 system of astrophysical molecule CoH, using a suitable potential. The dissociation energy D
0
0 = 2.5 ± 0.05 eV for the electronic ground state of CoH has been estimated by fitting Hulburt-Hirschfelder function to the
experimental potential energy curve, using the correlation coefficient.
This revised version was published online in July 2006 with corrections to the Cover Date. 相似文献
4.
B. Karthikeyan V. Raja N. Rajamanickam S. P. Bagare 《Astrophysics and Space Science》2006,306(4):231-234
For molecular identification in astrophysical sources, an astrophysicist needs some spectroscopic parameters such as dissociation
energy, vibrational or rotational temperature of the source, band or line wavelengths, transition probability parameters,
etc. The Franck-Condon(FC) factors are proportional to the transition probabilities. In this study, the FC factors and r-centroids for the vibronic (vibration-electronic) transitions C
1 Σ + → X
1 Σ + of aluminium hydride (AlH), b
3 Σ ( −) → a
3 Π, C
1 Σ + → A
1 Π & C
′1 Δ → Δ 1 Π of boron hydride (BH) have been evaluated and the results are presented in tables which include band origin/head wavelengths.
The physical & astrophysical significances of our evaluated FC factors & r-centroids have been discussed and the possible presence of AlH in sunspot umbral spectra is also predicted.
PACS: 33 · 70 · Ca 相似文献
5.
High resolution FTS sunspot umbral spectra from NSO/Kitt Peak were used to detect rotational lines due to 11 electronic transitions of the molecule AlF, in the wavelength region 4400 – 9000 Å. The presence of lines due to bands C – A (0,0), (0,1), (0,2) and (1,2), D – A (0,0) and (0,1), F – A (0,0), G – A (0,0), and F – B (0,0) is confirmed. Further, the presence of lines due to C – A (1,0) and (1,1) transitions is treated as doubtful because of heavy blending in the region, by rotational lines of TiO. Among the identified lines, those which are well resolved were selected for measurement of equivalent widths. The measured values for the bands D – A (0,0) and F – A (0,0) were used to estimate the respective effective rotational temperatures to be 1240 ± 120 K and 2390 ± 400 K. 相似文献
6.
B. Viswanathan R. Shanmugavel S. P. Bagare N. Rajamanickam P. Sriramachandran 《Solar physics》2009,257(2):261-269
High-resolution Fourier transform spectrometer sunspot umbral spectra obtained at the National Solar Observatory/Kitt Peak
were used to identify molecular rotational lines arising from the infrared band systems of CrH and CrD molecules. Measurement
of the equivalent width used the Gaussian-profile approximation method, which is suitable especially for faint lines. Equivalent
widths are measured for an adequate number of best lines of the A – X (0,0) band of CrH and the A – X (0,0;1,0) bands of CrD
and, thereby, the effective rotational temperatures are estimated. 相似文献
7.
Jagdev Singh S. S. Hasan G. R. Gupta D. Banerjee S. Muneer K. P. Raju S. P. Bagare R. Srinivasan 《Solar physics》2009,260(1):125-134
We obtained the images of the eastern part of the solar corona in the Fe xiv 530.3 nm (green) and Fe x 637.4 nm (red) coronal emission lines during the total solar eclipse of 29 March 2006 at Manavgat, Antalya, Turkey. The images
were obtained using a 35 cm Meade telescope equipped with a Peltier-cooled 2k × 2k CCD and 0.3 nm pass-band interference filters
at the rates of 2.95 s (exposure times of 100 ms) and 2.0 s (exposure times of 300 ms) in the Fe xiv and Fe x emission lines, respectively. The analysis of the data indicates intensity variations at some locations with period of strongest
power around 27 s for the green line and 20 s for the red line. These results confirm earlier findings of variations in the
continuum intensity with periods in the range of 5 to 56 s by Singh et al. (Solar Phys.
170, 235, 1997). The wavelet analysis has been used to identify significant intensity oscillations at all pixels within our field of view.
Significant oscillations with high probability estimates were detected for some locations only. These locations seem to follow
the boundary of an active region and in the neighborhood, rather than within the loops themselves. These intensity oscillations
may be caused by fast magneto-sonic waves in the solar corona and partly account for heating of the plasma in the corona. 相似文献
8.
Singh Jagdev Cowsik R. Raveendran A. V. Bagare S. P. Saxena A. K. Sundararaman K. Krishan Vinod Naidu Nagaraja Samson J. P. A. Gabriel F. 《Solar physics》1997,170(2):235-252
An experiment to search for short-period oscillations in the solar corona was conducted during the total solar eclipse of 1995 October 24 at Kalpi, India. The intensity in the continuum, centred around 5500 Å and with a passband having a half-width of 240 Å, was recorded at a counting rate of 20 Hz using a thermoelectric-liquid cooled photomultiplier. The power-spectrum analysis of the data reveals that most of the power is contained in 6 frequencies below 0.2 Hz. A least-square analysis gives the periods of the 6 frequency components to be 56.5, 19.5, 13.5, 8.0, 6.1, and 5.3 s. These oscillations are found to be sinusoidal, and their amplitudes are found to lie in the rangeinebreak 0.2–1.3% of the coronal brightness. Assuming these oscillations to be fast magnetosonic modes, the calculations indicate the availability of enough flux for the heating of the active regions in the solar corona. 相似文献
9.
A search has been carried out for the presence of rotational lines of two bands of the (0, 0) and (1, 1) A 1Π?–?X 1Σ+ system of the AlH molecule in the high resolution Fourier Transform Spectra of sunspots observed at the National Solar Observatory at Kitt Peak. Though the presence of the AlH molecule in sunspots was confirmed by Wallace, Hinkle, and Livingston (An Atlas of Sunspot Umbral Spectra in the Visible from 15?000 to 25?000 cm?1 (3920 to 6664 Å), Tech. Rep. 00-001, National Solar Observatory, Tucson, AZ, 2000), there is no report on the rotational temperature in the literature by identifying AlH molecular lines. The results obtained in this new search using a suitable identification technique are compared with the results reported by Wallace, Hinkle, and Livingston (2000). In view of the fact that the rotational temperatures of the molecules could be used to test photospheric and sunspot models, the effective rotational temperature for the (0, 0) band of the A?–?X system of AlH molecule is estimated by measuring the equivalent widths of well resolved spectral lines and its value justifies the existence of the AlH molecule in sunspots. 相似文献
10.
P. Sriramachandran R. Shanmugavel S. P. Bagare N. Rajamanickam 《Astrophysics and Space Science》2009,323(1):41-49
A high resolution spectrum of a sunspot umbra is used for identification of rotational lines due to (0, 0) band of the A
2Π–X
2Σ+ system and (0, 0), (1, 1), and (2, 2) bands of the B
2Σ+–X
2Σ+ system of the molecule SrF. The published sunspot umbral spectrum obtained with Fourier Transform Spectrometer and solar
telescope of National Solar Observatory/National Optical Astronomy Observatory at Kitt Peak was used for the study. The new
identification of more than 200 SrF lines in the umbral spectrum confirms that this molecule accounts for the majority of
lines in the spectral range 15050 to 15360 cm−1 and 17240 to 17300 cm−1. Equivalent widths have been measured for well-resolved lines of these bands and the effective rotational temperatures have
been estimated for which the presence is confirmed. 相似文献