A study of dust structure nearby white dwarf  WD1334-678

Joshi, Ishwor Nath; Jha, Alok; Aryal, B.

doi:10.3126/bibechana.v18i2.37439

Cited by 3 publications

(5 citation statements)

References 12 publications

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“…The same trend is followed in this work also; the Gaussian distribution deviated slightly in IRIS (I1) and AKARI (A1 and A2) data but deviated heavily in the WISE data (W1 and W2), which might be due to the presence of the Supernova Remnants at the center of the dust structures. The range of temperature in the cavity structure nearby the White Dwarf WD 1334-678 is 17.70 K to 18.81 K in AKARI data [25], which is quite lower value in comparison to the temperature obtained in this work in AKARI data, possibly due to the nebular structure. Also, the mass of dust per pixels around WD 1334-678 is 1.10×10 25 kg, which is larger compare to this work.…”

Section: Density and Jeans Masscontrasting

confidence: 77%

“… The analysis of background sources in the SIM-BAD database reveals several sources, in which the Supernova Remnants; SN 2008ce and SN 2010k are recognized at the center of the bipolar dust structure, which might be the important source of the dust as well as a contributor of energetic radiation responsible for the dust heating.  The mass of dust in isolated region is found to be 6.53×10 24 kg in I1, 1.66×10 26 kg in A1, 5.60×10 26 kg in A2, 5.48×10 25 kg in W1 and 6.32×10 25 kg in W2. The density of the dust is minimum in IRIS and maximum in WISE data.…”

Section: Density and Jeans Massmentioning

confidence: 93%

“…In W1 and W2, the infrared flux is smooth varying from center to outside, which is due to the higher resolution of WISE image than AKARI and IRIS image. The contour map of dust color temperature is different than the infrared flux and enclosing the 6.32 ×10 25 1.26 ×10 28 intricate infrared features. In I1, W1 and W2, the temperature is high towards the center, but in A1 and A2 it is less towards the center.…”

Section: Contour Map Of Infrared Flux Temperature and Massmentioning

confidence: 94%

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Comparative Study of Dust Properties around White Dwarf PG 1225-079 in IRIS, AKARI and WISE Data

Sigdel¹,

Rijal²,

Paudel³

2022

J. Nep. Phys. Soc.

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In this work, dust properties around the White Dwarf PG 1225-079 located at RA (J2000): 12h 27m 47.35s, DEC(J2000): -08° 14’ 37.97” is studied extensively using the publicly available data from Improved Reprocessing of IRAS Survey (IRIS), AKARI infrared survey and Wide field Infrared Survey Explorer (WISE). The bipolar dust structure hardly resolved in IRIS (60 μm and 100 μm) is clearly resolved in AKARI (90 μm and 140 μm) and WISE (12 μm and 22 μm) images. The dust color temperature and dust mass are calculated from the infrared flux density. The average value of dust color temperature in isolated dust structure is 27.57 K for IRIS (I1). For isolated upper and lower dust clouds the average temperatures are; 22.64 K and 22.63 K for AKARI (A1 and A2), 295.34 K and 296.85 K in WISE (W1 and W2) data. A wide range of temperatures suggests the bipolar dust structure is dynamically active. The mass of dust is found to be 3.44 × 1025 kg in IRIS (I1), 1.82 × 1026 kg and 5.89×1026 kg in two bipolar regions in AKARI (A1 and A2) and 1.12 ×1026 kg and 1.14×1026 kg in WISE (W1 and W2). A good relation is found between the infrared flux in all survey data with r2 value 0.83 in IRIS (I1) and more than 0.90 in AKARI (A1, A2) and WISE (W1, W2) data. SIMBAD database explore some sources including Supernova Remnants nearby the dust which might be the progenitor of dust as well as the contributor of energetic radiation. The Gaussian modeling of temperature is found to be deviated from normal shape. The contour plot of dust color temperature and dust mass shows non uniform variation among the IRIS, AKARI and WISE survey. The relation between infrared flux, dust color temperature and dust mass within the dust clouds are presented.

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Section: Density and Jeans Masscontrasting

confidence: 77%

Section: Density and Jeans Massmentioning

confidence: 93%

Section: Contour Map Of Infrared Flux Temperature and Massmentioning

confidence: 94%

See 1 more Smart Citation

Comparative Study of Dust Properties around White Dwarf PG 1225-079 in IRIS, AKARI and WISE Data

Sigdel¹,

Rijal²,

Paudel³

2022

J. Nep. Phys. Soc.

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“…studied far infrared (60 µm and 100 µm) IRAS loop at -5 o Galactic latitude around pulsar J1627-5547 by taking different dust properties like Dust Color Temperature, Dust Mass, and Inclination angle and they conclude that the results are agreed with Gaussian similar works are also done by Chaudhary et al (2022). Several research has been performed exploring the properties of interstellar dust using the infrared data in the region near the Pulsars [10,11] , White Dwarfs [12,13] , AGB Star [14,15] , Supernova Remnants [16] , FIR loops [17,18] , FIR Cavities [19] , etc., using the data from IRAS, IRIS, and AKARI. In this work, we have studied the multiwavelength variation of dust color temperature together with dust mass near the pulsar J0302+2252 using IRIS, AKARI, and WISE surveys.…”

Section: Introductionmentioning

confidence: 57%

Study of dust properties nearby pulsar J0302+2252 using Iris, Akari and wise surveys

Khatiwada¹,

Chaudhary²,

Subedi³

et al. 2023

IJMRGE

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A search of dust structure nearby the pulsar J0302+2252 in IRIS , AKARI and WISE survy was performed using Skyview Observatory (http://skyview.gsfc.nasa.gov). The physical properties have been studied at 60µm & 100µm in the IRIS survey, 90µm & 140µm in the AKARI survey and 12µm & 22µm in the WISE survey at right ascension (R.A.) (J2000)=30h(_^) 02m 31.99s and Declination (Decl.) (J2000)=+ 220 52m 12.10s . In this work, we have studied the physical properties such as Dust color temperature, Planck’s unction, Visual extinction and Mass profile of the dust data reduction software ALADIN v11. The dust color temperature is found to be 22.271 ± 0.261K in IRIS, 22.343 ± 0.939 K in AKARI and 278.74 ± 0.067 K in WISE. Also, the dust mass is found to be 2.286 × 1027 kg (1.149 × 10-3 M⊙ ) in IRIS, 8.800 ×1027 kg (0.416× 10-3 M⊙ ) in AKARI and 5.220 ×1025 kg (0.026 ×10-3 M⊙ ) in WISE. The average visual extinction is found to be 1.372 ×10-13 mag. In IRIS, 4.970 ×10-14 mag. In AKARI and 1.673 ×10-15 mag. In WISE. The dust color temperature and dust mass distribution show a very good agreement with Gaussian. The Contour plots of dust color temperature and dust mass show inverse relation between them in all three bands IRIS, AKARI, and WISE.

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“…In past, many research has been performed exploring the properties of interstellar dust using the infrared data in the region near the Pulsars [8,9], White Dwarfs [10,11], AGB Star [12,13], Supernova Remnants [14,15], FIR loops [16][17][18][, FIR Cavities [18,19], Isolated Nebula [20], etc., using the data from IRAS, IRIS and AKARI. In this work, we have used the data from IRIS and AKARI to explore the properties of dust within the molecular cloud.…”

Section: Introductionmentioning

confidence: 99%

Properties of dust in the North - East part of Perseus Cloud within the open cluster IC 348 using data from IRIS and AKARI

et al. 2023

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In this work, we have studied the dust properties of the North-East part of Perseus cloud having a size of 0.5o × 0.5o located at RA (ICRS): 56.14o DEC (ICRS): +32.15o, within the Open Cluster IC 348, using IRIS and AKARI data. An isolated region of size 0.39o×0.23o in IRIS and 0.34o×0.16o in AKARI data is detected within it. The infrared fluxes extracted using Aladin v11.0 are used to study the dust temperature and dust mass. The distance of the selected dust structure is calculated using Gaia EDR3, which is 309.98 pc. The infrared flux density is found to be increased for long-wavelength data. The average dust color temperature calculated from short-wavelength IRIS data is more than that calculated from long-wavelength AKARI data, which are 26.34 K±0.11 K for IRIS and 17.63 K±0.02 K for AKARI data. The mass of dust within the entire dust structure is 0.06 Mʘ for IRIS data and 37.44 Mʘ for AKARI data. Jeans mass for isolated region gives contradictory results in two surveys, for IRIS survey total mass is smaller than Jeans mass but for AKARI survey the total mass is larger than the Jeans mass. A good correlation between infrared fluxes is noticed for linear regression. The study background sources observed from the SIMBAD database explore the large number of stars, X-ray sources, YSOs, etc., embedded within the dust structure; some of them are responsible for dust heating and some for the contribution of dust mass. The contour map shows the identical distribution between infrared fluxes, dust color temperature and Planck’s function and dissimilar distribution between dust mass and visual extinction in IRIS and AKARI data. The high temperature at the central region suggests that the core of dust structure is thermally active, radiating the large thermal radiation in comparison to the outer region.

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A study of dust structure nearby white dwarf WD1334-678

Cited by 3 publications

References 12 publications

Comparative Study of Dust Properties around White Dwarf PG 1225-079 in IRIS, AKARI and WISE Data

Comparative Study of Dust Properties around White Dwarf PG 1225-079 in IRIS, AKARI and WISE Data

Study of dust properties nearby pulsar J0302+2252 using Iris, Akari and wise surveys

Properties of dust in the North - East part of Perseus Cloud within the open cluster IC 348 using data from IRIS and AKARI

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