Jayanand Maurya

@xao.ac.cn

Postdoctoral Fellow, Optical Astronomy Division
Xinjiang Astronomical Observatory, Chinese Academy of Sciences, Urumqi, China

Jayanand Maurya


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https://researchid.co/jayanand107

RESEARCH, TEACHING, or OTHER INTERESTS

Astronomy and Astrophysics, Physics and Astronomy
12

Scopus Publications

129

Scholar Citations

7

Scholar h-index

6

Scholar i10-index

Scopus Publications

  • The Impact of Stellar Rotations and Binaries on the Shape of Upper Main Sequence near Turnoff in Open Cluster NGC 6067
    Jayanand Maurya, Yu Zhang, Sebastian Kamann, Hubiao Niu, Yves Frémat, Kaixiang Lang, Y. C. Joshi, M. R. Samal, Peter De Cat, Ali Esamdin
    Astrophysical Journal, 2025
    We present the analysis of the extended main-sequence turnoff (eMSTO) in the open cluster NGC 6067. We derive the projected rotational velocity, vsini, of the stars belonging to the eMSTO region of the main sequence (MS) utilizing Gaia-ESO spectra. Our results reveal a positive correlation between vsini and the color of eMSTO stars, where fast-rotating stars predominantly occupy the red part of the MS while slow-rotating ones prefer a bluer side of the MS. The gravity-darkening effect might be a reason for this correlation. We find that most of the close binaries present in the eMSTO population would be slow-rotating due to the tidal-locking phenomenon. We identify four double-lined spectroscopic binaries (SB2) featuring slow-rotating companions, further supporting this tidal-locking hypothesis. However, the spatial distribution and the cumulative radial distribution indicate a higher concentration of red eMSTO stars in the cluster’s central region than their bluer counterparts. This suggests that tidal locking is less likely to be the cause of the observed spread in rotation rates among eMSTO stars. Instead, we propose that star–disk interactions during the pre-main-sequence phase might have played a crucial role in spreading the rotation rates of stars, leading to the eMSTO phenomenon in NGC 6067.
  • Insights into the 3D layered structure of nearby open clusters through N -body simulations
    Kaixiang Lang, Yu Zhang, Hubiao Niu, Jayanand Maurya, Jinzhong Liu, Guimei Liu
    Astronomy and Astrophysics, 2025
    Context. Open clusters (OCs) are important for understanding star formation, dynamics, and evolution. Previous studies have indicated a relationship between cluster structure and member star properties, but the formation mechanism of the layered structure of OCs remains unclear. Aims. We study the three-dimensional spatial distribution of 279 nearby OCs to understand the formation mechanism of the layered structure. Methods. We analyzed the spatial distribution of member stars within each OC and correlated the presence of a layered structure with the number of member stars. Additionally, we performd N-body simulations to model the evolution of OCSN 125. We assessd the correlation between the binary fraction, the most massive star, and the radius of the layered structure in each simulated OC. Results. Our analysis reveals that OCs with fewer member stars tend to lack a layered structure. The results from N-body simulations indicate that the presence of a layered structure is strongly influenced by dynamical factors, particularly the most massive star and the binary fraction. Massive stars drive mass loss through supernova explosions and stellar winds, which weaken the spatial layering. Furthermore, clusters with higher binary fractions exhibit a weaker layered structure, likely due to energy equipartition, dynamical friction, and perturbations caused by binary systems. These factors contribute to delaying core collapse and slowing the emergence of a layered structure. Conclusions. Our findings suggest that dynamical interactions, including the effects of the most massive stars and binary fraction, play a critical role in the formation and disruption of the layered structure in OCs.
  • Origin of extended main-sequence turn-off in open cluster NGC 2355
    Jayanand Maurya, M R Samal, Louis Amard, Yu Zhang, Hubiao Niu, Sang Chul Kim, Y C Joshi, B Kumar
    Monthly Notices of the Royal Astronomical Society, 2024
    The presence of extended Main-Sequence Turn-Off (eMSTO) in the open clusters has been attributed to various factors, such as spread in rotation rates, binary stars, and dust-like extinction from stellar excretion discs. We present a comprehensive analysis of the eMSTO in the open cluster NGC 2355. Using spectra from the Gaia–European Southern Observatory (ESO) archives, we find that the stars in the red part of the eMSTO have a higher mean v sin i value of 135.3 $\\pm$ 4.6 km s$^{-1}$ compared to the stars in the blue part that have an average v sin i equal to 81.3 $\\pm$ 5.6 km s$^{-1}$. This suggests that the eMSTO in NGC 2355 is possibly caused by the spread in rotation rates of stars. We do not find any substantial evidence of the dust-like extinction from the eMSTO stars using ultraviolet data from the Swift survey. The estimated synchronization time for low-mass ratio close binaries in the blue part of the eMSTO suggests that they would be mostly slow-rotating if present. However, the stars in the blue part of the eMSTO are preferentially located in the outer region of the cluster indicating that they may lack low-mass ratio close binaries. The spread in rotation rates of eMSTO stars in NGC 2355 is most likely caused by the star-disc interaction mechanism. The stars in the lower main sequence beyond the eMSTO region of NGC 2355 are slow rotating (mean v sin i = 26.5 $\\pm$ 1.3 km s$^{-1}$) possibly due to the magnetic braking of their rotations.
  • Statistical analysis of dynamical evolution of open clusters
    Jayanand Maurya, Y. C. Joshi, Manash Ranjan Samal, Vineet Rawat, Anubha Singh Gour
    Journal of Astrophysics and Astronomy, 2023
  • Investigating Stellar Variability in the Open Cluster Region NGC 381
    Jayanand Maurya, Y. C. Joshi, A. Panchal, A. S. Gour
    Astronomical Journal, 2023
    We study variable stars in the field of the open cluster NGC 381 using photometric data observed over 27 nights and identify a total of 57 variable stars, six of which are member stars. The variable stars are classified based on their periods, amplitudes, light-curve shapes, and locations in the H-R diagram. We found a rich variety of variable stars in the cluster. We identified a total of 10 eclipsing binaries, of which two are of Algol type while eight are of W UMa type (EW). The estimated ages of these EW binaries are greater than 0.6 Gyr, which is in agreement with the formation time constraint of ≥0.6 Gyr on short-period eclipsing binaries. The physical parameters of the two EW-type binaries are estimated using PHOEBE model-fitting software. The pulsating variable stars include one each from the δ Scuti and γ Dor variability classes. We determined the pulsation modes of pulsating variables with the help of the FAMIAS package. We obtained 15 rotational variable stars comprising four dwarf stars identified on the basis of their log(g) versus log(T eff) diagram. These dwarf stars are found to have generally longer periods than the remaining rotational variables.
  • Photometric and Kinematic Study of the Open Clusters SAI 44 and SAI 45
    Jayanand Maurya, Y. C. Joshi, W. H. Elsanhoury, Saurabh Sharma
    Astronomical Journal, 2021
    We carry out a detailed photometric and kinematic study of the poorly studied sparse open clusters SAI 44 and SAI 45 using ground-based BVR c I c data supplemented by archival data from Gaia eDR3 and Pan-STARRS. The stellar memberships are determined using a statistical method based on Gaia eDR3 kinematic data, and we found 204 members in SAI 44 while only 74 members are identified in SAI 45. The average distances to SAI 44 and SAI 45 are calculated to be 3670 ± 184 and 1668 ± 47 pc. The logarithmic age of the clusters are determined to be 8.82 ± 0.10 and 9.07 ± 0.10 yr for SAI 44 and SAI 45, respectively. The color–magnitude diagram of SAI 45 hosts an extended main-sequence turnoff (eMSTO). The apparent age spread is found to be similar to the apparent age spread predicted on the basis of the age spread and cluster age relation predicted by rotation models. This indicates that eMSTO is a stellar evolution rather than star formation phenomenon in SAI 45. We conclude that eMSTO in SAI 45 is mainly caused by the different rotation rates of stars as the SYCLIST synthetic population with different rotation rates was able to reproduce the observed eMSTO, and stars in the red part of the eMSTO were preferentially concentrated in the inner region, which again hints at different rotations being the reason for the extension in the upper MS. This finding supports the theory attributing the origin of eMSTO to the different rotations of eMSTO stars. The mass function slopes are obtained as −2.24 ± 0.66 and −2.58 ± 3.20 in the mass rages 2.426–0.990 M ⊙ and 2.167–1.202 M ⊙ for SAI 44 and SAI 45, respectively. SAI 44 exhibits the signature of mass segregation while we found weak evidence of mass segregation in SAI 45 possibly due to tidal stripping. The dynamical relaxation times of these clusters indicate that both clusters are in a dynamically relaxed state. Using the AD-diagram method, the apex coordinates are found to be ( 69 .° 79 ± 0 .° 11 , − 30 .° 82 ± 0 .° 15 ) for SAI 44 and (− 56 .° 22 ± 0 .° 13 , − 56 .° 62 ± 0 .° 13 ) for SAI 45. The average space velocity components of the clusters SAI 44 and SAI 45 are calculated in units of km s−1 as (−15.14 ± 3.90, −19.43 ± 4.41, −20.85 ± 4.57) and (28.13 ± 5.30, −9.78 ± 3.13, −19.59 ± 4.43), respectively.
  • Variable stars in the field of intermediate-age open cluster NGC559
    Y C Joshi, Ancy A John, J Maurya, A Panchal, Brijesh Kumar, Santosh Joshi
    Monthly Notices of the Royal Astronomical Society, 2020
    This work presents the first long-term photometric variability survey of the intermediate-age open cluster NGC 559. Time series V-band photometric observations on 40 nights taken over more than 3 yr with three different telescopes are analysed to search for variable stars in the cluster. We investigate the data for the periodicity analysis and reveal 70 variable stars including 67 periodic variables in the target field, all of them are newly discovered. The membership analysis of the periodic variables reveals that 30 of them belong to the cluster and remaining 37 are identified as field variables. Out of the 67 periodic variables, 48 are short-period (P < 1 d) variables and 19 are long-period (P > 1 d) variables. The variable stars have periodicity between 3 h to 41 d and their brightness ranges from V = 10.9 to 19.3 mag. The periodic variables belonging to the cluster are then classified into different variability types on the basis of observational properties such as shape of the light curves, periods, amplitudes, as well as their positions in the Hertzsprung–Russell (H–R) diagram. As a result, we identify 1 Algol type eclipsing binary, 1 possible blue straggler star, 3 slowly pulsating B type stars, 5 rotational variables, 11 non-pulsating variables, 2 FKCOM variables, and remaining 7 are characterized as miscellaneous variables. We also identify three eclipsing binary stars (EBs) belonging to the field star population. The phoebe package is used to analyse the light curve of all four EBs in order to determine the parameters of the binary systems such as masses, temperatures, and radii.
  • Photometric and kinematic study of the three intermediate age open clusters NGC 381, NGC 2360, and Berkeley 68
    Jayanand Maurya, Y C Joshi
    Monthly Notices of the Royal Astronomical Society, 2020
    We present UBVRcIc photometric study of three intermediate age open star clusters NGC 381, NGC 2360, and Berkeley 68 (Be 68). We examine the cluster membership of stars using recently released Gaia DR2 proper motions and obtain a total of 116, 332, and 264 member stars in these three clusters. The mean reddening of E(B − V) = 0.36 ± 0.04, 0.08 ± 0.03, and 0.52 ± 0.04 mag is found in the direction of these clusters where we observe an anomalous reddening towards NGC 381. We fitted the solar metallicity isochrones to determine age and distance of the clusters which are found to be log(Age) = 8.65 ± 0.05, 8.95 ± 0.05, and 9.25 ± 0.05 yr with the respective distance of 957 ± 152, 982 ± 132, and 2554 ± 387 pc for the clusters NGC 381, NGC 2360, and Be 68. A two-stage power law in the mass function (MF) slope is observed in the cluster NGC 381, however, we observe only a single MF slope in the clusters NGC 2360 and Be68. To study a possible spatial variation in the slope of MF, we estimate slopes separately in the inner and the outer regions of these clusters and notice a steeper slope in outer region. The dynamic study of these clusters reveals deficiency of low-mass stars in their inner regions suggesting the mass segregation process in all these clusters. The relaxation times of 48.5, 78.9, and 87.6 Myr are obtained for the clusters NGC 381, NGC 2360, and Be 68, respectively, which are well below to their respective ages. This suggests that all the clusters are dynamically relaxed.
  • Photometric, kinematic, and variability study in the young open cluster NGC1960
    Y C Joshi, J Maurya, A A John, A Panchal, S Joshi, B Kumar
    Monthly Notices of the Royal Astronomical Society, 2020
    We present a comprehensive photometric analysis of a young open cluster NGC 1960 (= M36) along with the long-term variability study of this cluster. Based on the kinematic data of Gaia DR2, the membership probabilities of 3871 stars are ascertained in the cluster field among which 262 stars are found to be cluster members. Considering the kinematic and trigonometric measurements of the cluster members, we estimate a mean cluster parallax of 0.86 ± 0.05 mas and mean proper motions of μRA = −0.143 ± 0.008 mas yr−1 and μDec. = −3.395 ± 0.008 mas yr−1. We obtain basic parameters of the cluster such as E(B − V) = 0.24 ± 0.02 mag, log(Age/yr) = 7.44 ± 0.02, and d = 1.17 ± 0.06 kpc. The mass function slope in the cluster for the stars in the mass range of 0.72–7.32 M⊙ is found to be γ = −1.26 ± 0.19. We find that mass segregation is still taking place in the cluster which is yet to be dynamically relaxed. This work also presents first high-precision variability survey in the central 13 arcmin × 13 arcmin region of the cluster. The V-band photometric data accumulated on 43 nights over a period of more than 3 yr reveals 76 variable stars among which 72 are periodic variables. Among them, 59 are short period (P < 1 d) and 13 are long period (P > 1 d). The variable stars have V magnitudes ranging between 9.1 to 19.4 mag and periods between 41 min and 10.74 d. On the basis of their locations in the H–R diagram, periods, and characteristic light curves, 20 periodic variables belong to the cluster are classified as 2 δ-Scuti, 3 γ-Dor, 2 slowly pulsating B stars, 5 rotational variables, 2 non-pulsating B stars, and 6 as miscellaneous variables.
  • Photometric study of the young open clusters ic 1442, king 21, and trumpler 7
    Jayanand Maurya, Y C Joshi, A S Gour
    Monthly Notices of the Royal Astronomical Society, 2020
    We carried out the UBVRcIc photometric study of three poorly studied young open clusters IC 1442, King 21, and Trumpler 7 (Tr 7). We obtained 263, 244, and 128 member stars using Gaia Data Release 2 proper motions and parallaxes in IC 1442, King 21, and Tr 7, respectively. The reddening, E(B − V), was derived to be 0.54 ± 0.04, 0.76 ± 0.06, and 0.38 ± 0.04 mag for these clusters. The comparison of observed colour–magnitude diagrams with solar metallicity isochrones yields log(age) = 7.40 ± 0.30, 7.70 ± 0.20, and 7.85 ± 0.25 yr and corresponding distances of 2847 ± 238, 2622 ± 156, and 1561 ± 74 pc for IC 1442, King 21, and Tr 7, respectively. The estimated mass function (MF) slopes are found to be −1.94 ± 0.18, −1.54 ± 0.32, and −2.31 ± 0.29 for IC 1442, King 21, and Tr 7, respectively. The study of MF slopes done separately in the inner and the outer regions of these clusters gives a steeper slope in the outer region, which suggests spatial variation in slope and mass segregation in the clusters. We found evidence of mass segregation after the dynamical study in these clusters. The obtained relaxation time, TE, is 74, 26, and 34 Myr for the clusters IC 1442, King 21, and Tr 7, respectively. The mass segregation in IC 1442 may be caused by early dynamical relaxation. The estimated TE is well below the ages of King 21 and Tr 7, which indicates that these clusters are dynamically relaxed.
  • Photometric study of the open cluster NGC 381
    Jayanand Maurya, Yogesh Chandra Joshi
    Bulletin De La Societe Royale Des Sciences De Liege, 2019
  • Optical characterization and Radial velocity monitoring of Exoplanet and Eclipsing Binary candidates
    Yogesh Chandra Joshi, Peter De Cat, Alaxendra Panchal, Aruna Goswami, Patricia Lampens, Lore Vermeylen, Jayanand Maurya
    Bulletin De La Societe Royale Des Sciences De Liege, 2019

RECENT SCHOLAR PUBLICATIONS

  • Unraveling eMSTO in NGC 2355: Stellar Rotation and Binaries
    J Maurya, Y Zhang, H Niu
    arXiv preprint arXiv:2511.12496 , 2025
    2025
  • The Impact of Stellar Rotations and Binaries on the Shape of Upper Main Sequence near Turnoff in Open Cluster NGC 6067
    J Maurya, Y Zhang, S Kamann, H Niu, Y Frémat, K Lang, YC Joshi, ...
    The Astrophysical Journal 989 (1), 123 , 2025
    2025
    Citations: 2
  • Insights into the 3D layered structure of nearby open clusters through N-body simulations
    K Lang, Y Zhang, H Niu, J Maurya, J Liu, G Liu
    Astronomy & Astrophysics 697, A122 , 2025
    2025
    Citations: 1
  • Origin of extended main-sequence turn-off in open cluster NGC 2355
    J Maurya, MR Samal, L Amard, Y Zhang, H Niu, SC Kim, YC Joshi, ...
    Monthly Notices of the Royal Astronomical Society 532 (1), 1212-1222 , 2024
    2024
    Citations: 7
  • Origin of extended Main Sequence Turn Off in open cluster NGC
    J Maurya, MR Samal, L Amard, Y Zhang, H Niu, SC Kim, YC Joshi, ...
    2024
  • Statistical analysis of dynamical evolution of open clusters
    J Maurya
    Journal of Astrophysics and Astronomy 44, 71 , 2023
    2023
    Citations: 10
  • VizieR Online Data Catalog: Study of NGC 381, NGC 2360 and Berkeley 68 (Maurya+, 2020)
    J Maurya, YC Joshi
    VizieR Online Data Catalog 749, J/MNRAS/494/4713 , 2023
    2023
  • VizieR Online Data Catalog: Study of the young open cluster NGC 1960 (Joshi+, 2020)
    YC Joshi, J Maurya, AA John, A Panchal, S Joshi, B Kumar
    VizieR Online Data Catalog 749, J/MNRAS/492/3602 , 2023
    2023
  • Investigating stellar variability in the open cluster region NGC 381
    J Maurya, YC Joshi, A Panchal, AS Gour
    The Astronomical Journal 165 (3), 90 , 2023
    2023
    Citations: 3
  • Statistical analysis of dynamical evolution of open clusters
    YC JOSHI, J MAURYA, V RAWAT, AS GOUR, MR SAMAL
    Journal Astrophysical Astronomy , 2023
    2023
  • Photometric Study of the Open Clusters SAI 44 and SAI 45
    J Maurya, YC Joshi
    44th COSPAR Scientific Assembly. Held 16-24 July 44, 596 , 2022
    2022
  • Photometric and kinematic study of the open clusters SAI 44 and SAI 45
    J Maurya, YC Joshi, WH Elsanhoury, S Sharma
    The Astronomical Journal 162 (2), 64 , 2021
    2021
    Citations: 14
  • Photometric, kinematic, and variability study in the galactic open clusters
    J Maurya
    ARIES, Nainital , 2021
    2021
  • Variable stars in the field of intermediate-age open cluster NGC 559
    YC Joshi, AA John, J Maurya, A Panchal, B Kumar, S Joshi
    Monthly Notices of the Royal Astronomical Society 499 (1), 618-630 , 2020
    2020
    Citations: 11
  • Photometric study of the young open clusters IC 1442, King 21, and Trumpler 7
    J Maurya, YC Joshi, AS Gour
    Monthly Notices of the Royal Astronomical Society 495 (2), 2496-2508 , 2020
    2020
    Citations: 15
  • Photometric and kinematic study of the three intermediate age open clusters NGC 381, NGC 2360, and Berkeley 68
    J Maurya, YC Joshi
    Monthly Notices of the Royal Astronomical Society 494 (4), 4713-4729 , 2020
    2020
    Citations: 28
  • Photometric, kinematic, and variability study in the young open cluster NGC 1960
    YC Joshi, J Maurya, AA John, A Panchal, S Joshi, B Kumar
    Monthly Notices of the Royal Astronomical Society 492 (3), 3602-3621 , 2020
    2020
    Citations: 33
  • Photometric, kinematic, and variability study in the young open cluster NGC1960
    B Kumar, J Maurya, YC Joshi, AA John, A Panchal, S Joshi
    Oxford University Press , 2020
    2020
  • Photometric study of the open cluster NGC 381
    J Maurya, YC Joshi
    Bulletin De La Societe Royale Des Sciences De Liege 88, 291-294 , 2019
    2019
    Citations: 3
  • Optical characterization and Radial velocity monitoring of Exoplanet and Eclipsing Binary candidates
    YC Joshi, P De Cat, A Panchal, A Goswami, P Lampens, L Vermeylen, ...
    Societe Royale des Sciences de Liege , 2019
    2019
    Citations: 2

MOST CITED SCHOLAR PUBLICATIONS

  • Photometric, kinematic, and variability study in the young open cluster NGC 1960
    YC Joshi, J Maurya, AA John, A Panchal, S Joshi, B Kumar
    Monthly Notices of the Royal Astronomical Society 492 (3), 3602-3621 , 2020
    2020
    Citations: 33
  • Photometric and kinematic study of the three intermediate age open clusters NGC 381, NGC 2360, and Berkeley 68
    J Maurya, YC Joshi
    Monthly Notices of the Royal Astronomical Society 494 (4), 4713-4729 , 2020
    2020
    Citations: 28
  • Photometric study of the young open clusters IC 1442, King 21, and Trumpler 7
    J Maurya, YC Joshi, AS Gour
    Monthly Notices of the Royal Astronomical Society 495 (2), 2496-2508 , 2020
    2020
    Citations: 15
  • Photometric and kinematic study of the open clusters SAI 44 and SAI 45
    J Maurya, YC Joshi, WH Elsanhoury, S Sharma
    The Astronomical Journal 162 (2), 64 , 2021
    2021
    Citations: 14
  • Variable stars in the field of intermediate-age open cluster NGC 559
    YC Joshi, AA John, J Maurya, A Panchal, B Kumar, S Joshi
    Monthly Notices of the Royal Astronomical Society 499 (1), 618-630 , 2020
    2020
    Citations: 11
  • Statistical analysis of dynamical evolution of open clusters
    J Maurya
    Journal of Astrophysics and Astronomy 44, 71 , 2023
    2023
    Citations: 10
  • Origin of extended main-sequence turn-off in open cluster NGC 2355
    J Maurya, MR Samal, L Amard, Y Zhang, H Niu, SC Kim, YC Joshi, ...
    Monthly Notices of the Royal Astronomical Society 532 (1), 1212-1222 , 2024
    2024
    Citations: 7
  • Investigating stellar variability in the open cluster region NGC 381
    J Maurya, YC Joshi, A Panchal, AS Gour
    The Astronomical Journal 165 (3), 90 , 2023
    2023
    Citations: 3
  • Photometric study of the open cluster NGC 381
    J Maurya, YC Joshi
    Bulletin De La Societe Royale Des Sciences De Liege 88, 291-294 , 2019
    2019
    Citations: 3
  • The Impact of Stellar Rotations and Binaries on the Shape of Upper Main Sequence near Turnoff in Open Cluster NGC 6067
    J Maurya, Y Zhang, S Kamann, H Niu, Y Frémat, K Lang, YC Joshi, ...
    The Astrophysical Journal 989 (1), 123 , 2025
    2025
    Citations: 2
  • Optical characterization and Radial velocity monitoring of Exoplanet and Eclipsing Binary candidates
    YC Joshi, P De Cat, A Panchal, A Goswami, P Lampens, L Vermeylen, ...
    Societe Royale des Sciences de Liege , 2019
    2019
    Citations: 2
  • Insights into the 3D layered structure of nearby open clusters through N-body simulations
    K Lang, Y Zhang, H Niu, J Maurya, J Liu, G Liu
    Astronomy & Astrophysics 697, A122 , 2025
    2025
    Citations: 1
  • Unraveling eMSTO in NGC 2355: Stellar Rotation and Binaries
    J Maurya, Y Zhang, H Niu
    arXiv preprint arXiv:2511.12496 , 2025
    2025
  • Origin of extended Main Sequence Turn Off in open cluster NGC
    J Maurya, MR Samal, L Amard, Y Zhang, H Niu, SC Kim, YC Joshi, ...
    2024
  • VizieR Online Data Catalog: Study of NGC 381, NGC 2360 and Berkeley 68 (Maurya+, 2020)
    J Maurya, YC Joshi
    VizieR Online Data Catalog 749, J/MNRAS/494/4713 , 2023
    2023
  • VizieR Online Data Catalog: Study of the young open cluster NGC 1960 (Joshi+, 2020)
    YC Joshi, J Maurya, AA John, A Panchal, S Joshi, B Kumar
    VizieR Online Data Catalog 749, J/MNRAS/492/3602 , 2023
    2023
  • Statistical analysis of dynamical evolution of open clusters
    YC JOSHI, J MAURYA, V RAWAT, AS GOUR, MR SAMAL
    Journal Astrophysical Astronomy , 2023
    2023
  • Photometric Study of the Open Clusters SAI 44 and SAI 45
    J Maurya, YC Joshi
    44th COSPAR Scientific Assembly. Held 16-24 July 44, 596 , 2022
    2022
  • Photometric, kinematic, and variability study in the galactic open clusters
    J Maurya
    ARIES, Nainital , 2021
    2021
  • Photometric, kinematic, and variability study in the young open cluster NGC1960
    B Kumar, J Maurya, YC Joshi, AA John, A Panchal, S Joshi
    Oxford University Press , 2020
    2020